Table of contents

The 23rd European Cosmic Ray Symposium (ECRS) took place in Moscow at the Lomonosov Moscow State University (3–7 July 2012), and was excellently organized by the Skobeltsyn Institute of Nuclear Physics of the Lomonosov Moscow State University, with the help of the Russian Academy of Sciences and the Council on the Complex Problem of Cosmic Rays of the Russian Academy of Sciences.

The first symposia were held in 1968 in Lodz, Poland (high energy, extensive air showers and astrophysical aspects) and in Bern (solar and heliospheric phenomena) and the two 'strands' joined together in 1976 with the meeting in Leeds. Since then the symposia, which have been very successful, have covered all the major topics with some emphasis on European collaborations and on meeting the demands of young scientists. Initially, a driving force was the need to overcome the divisions caused by the 'Cold War' but the symposia continued even when that threat ceased and they have shown no sign of having outlived their usefulness.

2012 has been an important year in the history of cosmic ray studies, in that it marked the centenary of the discovery of enigmatic particles in the perilous balloon ascents of Victor Hess. A number of conferences have taken place in Western Europe during the year, but this one took place in Moscow as a tribute to the successful efforts of many former USSR and other Eastern European scientists in discovering the secrets of the subject, often under very difficult conditions.

The symposium covers a wide range of scientific issues divided into the following topics:

On a personal note, as I step down as co-founder and chairman of the International Advisory Committee, I should like to thank those very many colleagues and friends with whom I have had the pleasure of working over the past 45 years. These thanks are extended to the present organizers.

The organizers are very grateful to the Russian Foundation of Basic Research and to the Dynasty non-profit foundation for financial support.

Arnold Wolfendale

All papers published in this volume of Journal of Physics: Conference Series have been peer reviewed through processes administered by the proceedings Editors. Reviews were conducted by expert referees to the professional and scientific standards expected of a proceedings journal published by IOP Publishing.

Centenaries provide useful perspectives for looking back upon long-past events and on their later consequences, and also on the activities of persons who made a lasting impact on some important field of research. Cosmic ray physics, as we now know it, had multiple roots. The most important puzzle that incited research in the early 20th century, however, was connected with the lack of understanding of the origin of an omnipresent extremely penetrating ionizing radiation. At least in hindsight, the balloon ascent of Victor Hess on the 7th August 1912 provided the first convincing evidence for the cosmic origin of that radiation, although Werner Kolhörster's subsequent flights to even higher altitudes and with better instrumentation certainly provided important confirmation. General acceptance of the existence of that radiation came more than a decade later, and its basic properties were revealed only in the early 30's. It was at about that time that a research student of Kolhörster, Lajos Jánossy, who happened to be borne in the discovery year of 1912, started his research in cosmic ray physics. Later he did important research in London, Manchester and Dublin, and wrote one of the first comprehensive monographs on cosmic rays. After his return to Hungary in 1950, he played an important part in establishing cosmic ray research in a newly formed research institute in Budapest.

The case is made for there being more 'structure' in the cosmic ray energy spectra than just the well-known knee at several PeV and the ankle at several EeV. Specifically, there seems to be a 'dip' or 'kink' at about 100 GeV/nucleon, a possible 'bump' at about 10 TeV, an 'iron peak' at 60 PeV and the possibility of further structure before the ankle is reached. The significance of the structures will be assessed.

In six years of data collection years in space, the experiment PAMELA has discovered very interesting features in cosmic rays, namely in the fluxes of protons, helium, electrons, that might change our basic vision of the mechanisms of production, acceleration and propagation of cosmic rays in the Galaxy. In addition, PAMELA measurements of cosmic antiproton and positron fluxes are setting strong constraints to the nature of Dark Matter. The continuous particle detection is allowing a constant monitoring of the solar activity and detailed study of the solar modulation for a long period, giving important improvements to the comprehension of the heliosphere mechanisms. PAMELA is also measuring the radiation environment around the Earth, and has recently discovered an antiproton radiation belt.

This review concentrates on the results obtained, over the last ten years, on the astrophysics of high-energy cosmic ray electrons and positrons. The anomalies, observed in the data of recent experiments (possible bump in the electron spectrum and the PAMELA anomaly in the positron fraction) are discussed through the systematic use of simple analytical solutions of the transport equations for cosmic ray electrons. Three main ways of explaining the origin of the anomalies are considered: the conservative way supposing the positrons to be pure secondary particles; the nearby sources like pulsars origin; and the dark matter origin. This review discusses, also, the inability to select the pulsars model or the dark matter model to explain the electron anomalies on the basis of the electron spectra with the usual large energy binning ( 15%). It is argued that the signature of nearby pulsars origin of the anomalies against the dark matter origin could be the fine structure of the cosmic ray electron spectrum predicted in the Malyshev et al. paper (2009) and which was observed in the data from the high-resolution ATIC experiment (2009-2011). To date, the high-resolution ATIC data was the only experimental result of this type published in the literature. Therefore, they should be tested by other experiments as soon as possible. Generally, there is, also, rather controversial situations between the data of the majority of recent experiments and, consequently, there is a noted urgent need for new high-precision and high-statistical experiments.

The detection of high-energy cosmic rays above a few hundred TeV is realized by the observation of extensive air-showers. By using the multi-detector setup of KASCADE-Grande, and here in particular the detectors of the large Grande array, the energy spectrum and the elemental composition of high-energy cosmic rays in the energy range from 10 PeV to 1 EeV are investigated. The estimation of energy and mass of the high-energy primary particles is based on the combined analysis of the total number of charged particles and the total number of muons measured by the detector arrays of Grande and KASCADE, respectively. The latest analysis results have shown that in the all-particle spectrum two features are present: a hardening of the spectrum at energies around 20 PeV and a steepening, i.e. a knee-like structure, at 80-90 PeV. The latter one was found to be due to a decrease of flux of the heavy mass component.

The IceCube Neutrino Observatory with its 1-km³ in-ice detector and the 1-km² surface detector (IceTop) constitutes a three-dimensional cosmic ray detector well suited for general cosmic ray physics. Various measurements of cosmic ray properties, such as energy spectra, mass composition and anisotropies, have been obtained from analyses of air showers at the surface and/or atmospheric muons in the ice.

The origin of the highest energy cosmic rays represents one of the most conspicuous enigmas of modern astrophysics, in spite of gigantic experimental efforts in the past fifty years, and of active theoretical research. The past decade has known exciting experimental results, most particularly the detection of a cut-off at the expected position for the long sought Greisen-Zatsepin-Kuzmin suppression as well as evidence for large scale anisotropies. This paper summarizes and discusses recent achievements in this field.

Currently the uncertainty in the prediction of shower observables for different primary particles and energies is dominated by differences between hadronic interaction models. The LHC data on minimum bias measurements can be used to test Monte Carlo generators and these new constrains will help to reduce the uncertainties in air shower predictions. In this article, after a short introduction on air showers we will show the results of the comparison between the updated version of high energy hadronic interaction models with LHC data. Results for air shower simulations and their consequence on the comparison with air shower data will be discussed.

Russian-Italian NEVOD-DECOR experiment on the measurements of the local muon density spectra (LMDS) at various zenith angles gave possibility to obtain information on primary cosmic ray flux and interaction characteristics in a record wide energy range from 10¹⁵ to more than 10¹⁸ eV. Comparison of the measurement results with CORSIKA-based simulations showed the increase of LMDS slope at PeV energies of primaries (corresponding to the first knee); a trend to a heavier primary mass composition above the knee; indication for a second knee (a further increase of the spectrum slope near 10¹⁷ eV). At large zenith angles and high muon densities (corresponding to primary energies around 10¹⁸ eV) a considerable excess of muon bundle events in comparison with the expectation based on independent estimates of the primary spectrum and widely used hadron interaction models has been found. In 2011, a new phase of measurements of the energy spectrum of cascade showers initiated by high-energy muons in water and of the energy deposit of muon bundles at various zenith angles and muon multiplicities started. Further plans include the deployment of a traditional EAS array around the NEVOD-DECOR complex.

Measurements of atmospheric Extensive Air Showers (EAS) are the only way of experimental studies of Primary Cosmic Rays (CR) with energies above 10¹⁵ eV. The final targets of these studies are search for astrophysical origin of these particles and properties of particle production in high energy particle interaction. Works presented at the PCR 2 session in the form of posters reflected the current progress in this area. In this review presented posters were grouped according to CR energy range, astrophysical significance, relation to high energy physics interaction properties and interaction models, and future experiments. 42 posters were submitted for this session. Some of the presented material in posters overlapped in parts with oral presentations.

The observation of gamma-ray sources at energies between tens of GeV and tens of TeV has been driven by ground-based Cherenkov telescopes. The observational techniques and methods employed have been continuously refined in the past years and have lead to the discovery of a steadily growing number of sources and source types. Similar to other branches of observational Astrophysics in the past, the field undergoes currently a transition from a discovery-driven to an exploration-driven stage. In this context, recent developments are summarized and highlights are presented.

Cosmic ray acceleration and magnetic amplification in shell-type supernova remnants is shortly reviewed. The results on the modeling of broadband electromagnetic emission from supernova remnants are presented and compared with observations.

In this paper a short summary of the posters presented in the section of muons and neutrinos of ECRS2012 is presented.

IceCube is the first representative of the km³ class of neutrino telescopes and currently the most sensitive detector to high-energy neutrinos. Its main mission is to search for Galactic and extragalactic sources of high-energy neutrinos, but it is also an excellent detector for the investigation of a variety of other highly topical astrophysics and particle physics topics like supernovae, dark matter and neutrino oscillations. After an introduction to neutrino astronomy and neutrino telescopes, this article presents a selection of latest results from the IceCube neutrino detector with respect to searches for cosmic high-energy neutrino sources.

The solar energetic particle (SEP) populations of electrons and ions are highly variable in space and time, in intensity, energy, and composition. Over the last ~20 years advanced instrumentation onboard many spacecraft (e.g. ACE, Coronas, GOES, Hinode, RHESSI, SAMPEX, SDO, SOHO, STEREO, TRACE, Ulysses, Yokoh, to name a few) extended our ability to explore the characteristics of solar energetic particles by in-situ measurements in interplanetary space and by observing their source characteristics near the Sun by remote-sensing observation of electromagnetic emission over a wide frequency range. These measurements provide crucial information for understanding the sources of the particle populations and the acceleration and propagation processes involved. We are now able to measure intensity-time profiles and anisotropies, energy spectra, elemental and isotopic abundances, and the ionic charge of particles over an extended energy range of 0.01 to several 100 MeV/nuc and for a large dynamic range of particle intensities. Furthermore, multi-spacecraft in-situ observations at different solar longitudes and latitudes provide new insight into the acceleration and propagation processes of SEPs near the Sun and in interplanetary space. In this paper we present an overview of SEP observations, their implications for SEP acceleration and propagation processes, and discuss open questions.

The views of two research groups are presented on the progress achieved in understanding one specific class of the long-term variations of the galactic cosmic ray intensity, the variations due to the sunspot and magnetic cycles in the solar activity. The main observational features of both cycles and how they can be described and understood are discussed for the two–decade period (1980-2000) that we consider as normal for the development of both cycles for the second half of the 20–th century. The unusual features in the cosmic ray behavior observed during the long and deep minimum between solar cycles 23 and 24 (2008-2010) are also discussed.

Space weather effects have two links to research of energetic particles in space. First, the direct one, connected with the interaction of high energy cosmic particles including galactic, solar cosmic rays, as well as magnetospheric particles, with various materials as satellite systems, atmosphere, ionosphere, airplane systems, human body at high altitudes and in space. Second one, the indirect relations, is checking the relevance of possible forecasts of space weather phenomena according to the data of energetic particles both on the ground and on the satellites and space probes. We review few selected aspects of the second type of relations with references mainly to recent studies, namely (i) progress in description of selected quasi-periodicities in cosmic ray time series which are of potential use for space weather studies, (ii) status in the forecast of geoeffective and radiation storm alerts using signatures of ground-based observations, (iii) problem of relativistic electrons in the vicinity of Earth.

This rapporteur paper addresses the SH poster session titled "Energetic particles in the heliosphere (solar and anomalous CRs, GCR modulation)" of the 23rd European Cosmic Ray Symposium (ECRS) and the 32nd Russian Cosmic Ray Conference (RCRC). The 65 posters presented are tentatively divided into five sections: Instruments and Methods; Solar Energetic Particles; Short Term Variations; Long Term Variations; Heliosphere.

Strong electric fields inside thunderclouds give rise to enhanced fluxes of high- energy electrons and, consequently, gamma rays and neutrons. During thunderstorms at Mount Aragats, hundreds of Thunderstorm Ground Enhancements (TGEs) comprising millions of energetic electrons and gamma rays, as well as neutrons, were detected at Aragats Space Environmental Center (ASEC) on 3200 m altitude. Observed large TGE events allow for the first time to measure the energy spectra of electrons and gamma rays well above the cosmic ray background. The energy spectra of the electrons have an exponential shape and extend up to 30-40 MeV. Recovered energy spectra of the gamma rays is also exponential in energy range 5-10 MeV, then turns to power law and extends up to 100 MeV.

Although it is generally believed that the increase in the mean global surface temperature since industrialisation is caused by the increase in green house gases in the atmosphere, some people cite solar activity, either directly or through its effect on cosmic rays, as an underestimated contributor to such global warming. In this paper a simplified version of the standard picture of the role of greenhouse gases in causing the global warming since industrialisation is described. The conditions necessary for this picture to be wholly or partially wrong are then introduced. Evidence is presented from which the contributions of either cosmic rays or solar activity to this warming is deduced. The contribution is shown to be less than 10% of the warming seen in the twentieth century.

This work is about neutron astronomy. The registration of high energy neutrons can be used to investigate gas and dust components of the Kuiper belt. A new method for studying the diffuse matter in space based on observing high energy neutrons is analyzed. The high energy neutrons (with energies of hundreds of Gev) can travel distances comparable to the distance between the Earth and the Kuiper belt. A background of neutrons (at these energies) from beyond the Solar System is limited by decay. It is shown that the expected flux of high energy neutrons can be recorded by facilities using the data on the density of the gas and dust component obtained when analyzing the trajectories of space probes.

Recent measurements of cosmic gamma ray intensities up to TeV energies have been used to estimate the spectral shape of the parent cosmic ray particles present in the interstellar medium. The case is made for the particle spectrum in the Inner Galaxy being flatter than locally and in the Outer Galaxy. Of various possible explanations we make the case for the propagation of the particles being different in the more turbulent interstellar medium of the Inner Galaxy. The characteristic parameter α for the so called anomalous diffusion is expected to be less in the Inner Galaxy than locally by about 0.2 and the corresponding power law spectral exponent of the cosmic ray particles differs from that locally by about Δ_γ 0.1.

This work is devoted to the calculation of the fluxes of the atmospheric antiprotons and antineutrons generated at various atmospheric depths, lying from 5 to 300 g/cm². The simulations are carried out with the help of CORSIKA package involving a primary energy spectrum starting at the energy threshold of antiparticle production up to 1 PeV. The obtained results match well with the atmospheric antiproton spectra measured by the BESS-2001 experiment in the kinetic energy range 1-3 GeV.

Isotopic anomalies of xenon in the nanodiamonds of chondrites testify to the rigid radiation and magneto hydrodynamic conditions at the last supernova explosion prior to formation of the Solar system.

We study the production of cosmic rays (CRs) in supernova remnants (SNRs), including the production of electron and positron CR components. This combines for the first time nuclear collisions inside CR sources and in the diffuse interstellar medium leading to the creation of electrons and positrons, as well as their reacceleration, with the injection and subsequent acceleration of suprathermal protons and electrons from the postshock thermal pool. Selfconsistent CR spectra are calculated on the basis of the nonlinear kinetic model. It is shown that reacceleration of positrons created in SNR and ISM produces a considerable effect at energies above 10 GeV, making its energy spectrum substantially flatter than the spectrum created in ISM. Calculated electron and positron spectra are in the satisfactory agreement with the existing measurements.

The CALorimetric Electron Telescope (CALET) will be installed on the Exposure Facility of the Japanese Experiment Module (JEM-EF) on the International Space Station (ISS) in 2014 where it will measure the cosmic-ray fluxes for five years. Its main scientific goals are to search for dark matter, investigate the mechanism of cosmic-ray acceleration and propagation in the Galaxy and discover possible astrophysical sources of high-energy electrons nearby the Earth. The instrument, under construction, consists of two layers of segmented plastic scintillators for the cosmic-ray charge identification (CHD), a 3 X₀-thick tungsten-scintillating fiber imaging calorimeter (IMC) and a 27 X₀-thick lead-tungstate calorimeter (TASC). The CHD can provide single-element separation in the interval of atomic number Z from 1 to 40, while IMC and TASC can measure the energy of cosmic-ray particles with excellent resolution in the range from few GeV up to several hundreds of TeV. Moreover, IMC and TASC provide the longitudinal and lateral development of the shower, a key issue for good electron/hadron discrimination. In this paper, we will review the status of the mission, the instrument configuration and its expected performance, and the CALET capability to measure the different components of the cosmic radiation.

This work analyzes the most probable mechanisms of the production of leading π⁰-mesons in gamma families. It was shown that major contribution to the generation of leading neutral mesons is made by the process of non-elastic recharging of an incident pion.

We propose a model where a supernova explodes in some vicinity of our solar system (some tens of parsecs) in the recent past (some tens of thousands years) with the energy release in cosmic rays of order of 10⁵¹ erg. The flux from this supernova is added to an isotropic flux from other sources. We consider the case where the Sun's location is not in some typical for Our Galaxy average environment, but in the Local Superbubble about 100 pc across, in which the diffusion coefficient D(E) = D₀ × E^0.6, with the value of D₀ ~ 10²⁵ cm² s⁻¹. We describe the energy dependence of the anisotropy of cosmic rays in the TeV region, together with the observed features of the energy spectrum of protons found in direct measurements. Our model provides a natural explanation to the hardening of the proton spectrum at 200 GeV, together with the observed steepening of the spectrum above 50 TeV.

The PAMELA project is the satellite experiment for measurements of the cosmic ray energy spectra in a wide energy range in near-Earth space. The PAMELA apparatus is in orbit from 2006 till today. The calorimeter is the main part of the instrument. It is able to measure energy, to distinguish between hadrons and electrons and to reconstruct the arriving particle direction. Using of special triggers for the calorimeter allows significant increasing of statistics. In consideration of these facts the technique of anisotropy searching in the energy range extending higher than 10 GeV has been developed. This technique is based on the calorimeter data and has as content the advanced method of the reconstruction of the secondary particle shower axis in the calorimeter.

On the 15th of June 2006, the PAMELA satellite-borne experiment was launched from the Baikonur cosmodrome and it has been collecting data since July 2006. The apparatus comprises a time-of-flight system, a silicon-microstrip magnetic spectrometer, a silicon-tungsten electromagnetic calorimeter, an anti-coincidence system, a shower tail counter scintillator and a neutron detector. The scientific objectives addressed by the mission are the measurement of the antiprotons and positrons spectra in cosmic rays, the hunt for antinuclei as well as the determination of light nuclei fluxes from hydrogen to oxygen in a wide energy range and with very high statistics. In this paper the identification capability for light nuclei isotopes (especially lithium and beryllium) using multiple dE/dx measurements in the calorimeter and first results of the isotopic ratio will be presented.

The study of cosmic ray physic of 10¹² – 10¹⁵ primary cosmic energy is one of the main goals of ARGO-YBJ experiment. The detector, located at the Yangbajing Cosmic Ray Laboratory (Tibet, 4300 m a.s.l., 606 g/cm²), is an EAS array consisting of a continuous carpet of RPCs. The low energy threshold of the detector allows to study an energy region characterized by the transition from the direct to the indirect measurements. In this talk we will report on the measurement of the cosmic ray energy spectrum at different zenith angles. The phenomenology of horizontal air shower (θ > 70°) will be described and discussed.

The silicon microstrip Tracker is a key subdetector of the AMS-02 instrument, designed to measure the momentum and charge of cosmic rays. The subdetector is composed of 9 layers of silicons sensors inside a permanent 0.15 T magnetic field. The detector has been installed on board of the International Space Station, at an altitude of 400 km, and is taking data since May 19th 2011. AMS-02 aims to provide a precise measurement of the cosmic-ray spectrum and perform antimatter searches in the GeV-TeV energy range. This review presents the Tracker performances during the first year of operation in space, covering all the most relevant aspects of detector stability, efficiency and capabilities in charge and track reconstruction.

The lateral distribution function (LDF) of extensive air shower (EAS)s play an important role in the analysis of the shower events and the particle content in it. These studies involve a collection of experimental works which at times turns out to be tedious. In many situations, while studying EAS, reconstruction of its constituents become important usually carried out using certain traditional approaches. Artificial Neural Network (ANN) can be used in these cases because of the fact that these are non-parametric tools with the ability to learn from the environment and use the knowledge for subsequent stages. Here, we propose a system based on ANN which is configured to accept high energy EAS shower sizes as an input parameter and provide the lateral distributions of the electronic component of the shower upto certain distance. A feedforward ANN is trained for the purpose which acts as a reliable system for estimating LDF for a range of shower events between 10^19.5 to 10^20.5 eV of primary energy.

The characteristics of the thermal neutrons flux have been measured near the EAS core at the "Carpet-2" EAS array. The thermal neutron detectors were placed on the floor of the tunnel of the Muon Detector (MD) and showers with a core near the MD were selected. Thermal neutrons multiplicity spectrum has been obtained for these showers. Measurements of the lateral distribution function of thermal neutrons at distances of 1-16 m from the shower axis have been performed. The mean number of the recorded thermal neutrons as a function of the number of hadrons crossing the MD has been measured.

The PAMELA experiment is carried out on board of the satellite Resurs DK1 launched on June 15th 2006 on polar orbit (the inclination is 70, the altitude is 350-600 km). The instrument which consists of magnetic spectrometer, silicon-tungsten imaging electromagnetic calorimeter gives a possibility to measure electron and positron fluxes over wide energy range from hundreds MeVs to hundreds GeVs. Measurements made in June 2006- January 2010 are presented and compared with other results and models. Positron spectrum appears to be harder than standard diffusive propagation models predict.

The ratios of fluxes of heavy nuclei from sulfur (Z=16) to chromium (Z=24) to the flux of iron were measured by the ATIC-2 experiment. The ratios are decreasing functions of energy from 5 GeV/n to approximately 80 GeV/n, as expected. However, an unexpected sharp upturn in the ratios are observed for energies above 100 GeV/n for all elements from Z=16 to Z=24. Similar upturn but with lower amplitude was also discovered in the ATIC-2 data for the ratio of fluxes of abundant even nuclei (C, O, Ne, Mg, Si) to the flux of iron. Therefore the spectrum of iron is significantly different from the spectra of other abundant even nuclei.

It is argued that the upturn observed in heavy nuclei to iron ratios as measured in the ATIC experiment could be understood within the model of closed galaxy with embedded local regions containing the sources of CR (Peters, Westergaard, 1977). The universal upturn near the energies of 200-300 GeV/n in the spectra of abundant primary nuclei is also predicted by this model, but it also predicts the source spectral index to be near 2.5.

Launched on the 15th of June 2006, the space experiment PAMELA is providing data showing interesting features in cosmic rays that might change our basic vision of the mechanisms of production, acceleration and propagation of cosmic rays in the galaxy. In addition, PAMELA measurements of cosmic antiproton and positron fluxes are setting strong constraints to the nature of Dark Matter. PAMELA is also testing cosmic rays acceleration and propagation models through precise measurements of light nuclei and their isotopes. The determination of fluxes and secondary-to-primary ratios is possible for nuclei up to Oxygen in the energy range 200MeV/n – 150 GeV/n. To investigate this important item, PAMELA can use measurements from three main detectors: the magnetic spectrometer, the calorimeter and the Time-of-Flight system. Analysis strategy and performance for nuclei studies using the detectors in stand-alone configuration will be discussed in this work.

The distribution of the cosmic-ray arrival direction provides essential information about the source distribution, the propagation medium and the diffusive process that primaries undergo. To the current knowledge of the local interstellar medium, cosmic rays in the rigidity range 10¹² – 10¹³ V are re-accelerated within few hundreds of astronomic units, what makes the TeV anisotropy an important probe to investigate the outer space until that horizon. We report the observation of anisotropy in the TeV cosmic-ray arrival direction measured with the ARGO-YBJ experiment, at angular scales in the range 10° – 180° and with intensity 10^−-4 – 10^−-3. Findings of other experiments are confirmed and new details on the cosmic-ray distribution in the declination range −10° – 70° are given.

Results of galactic deuteron spectrum measurement by means of PAMELA apparatus are described. PAMELA is an international experiment developed for antimatter search and measurement of p,He, electron and positron spectra in wide energy range. In addition, PAMELA allows to identify and measure deuteron spectrum at low energies. In this paper deuteron-to-proton ratio and deuteron spectrum are presented.

We have demonstrated a reasonably satisfactory agreement between the theoretically simulated geomagnetically confined antiproton fluxes and the Pamela experimentally observed antiproton fluxes within the Earth's magnetosphere. The antiprotons were considered created partially in nuclear reactions of direct proton/antiproton production (p+p, p+pbar+p+p) and to an even larger extent in nuclear reactions of neutron/antineutron (indirect) pair production (p+p, n+nbar+p+p) both processes resulting from cosmic rays interactions with the Earth's upper atmosphere. Although the theoretically predicted spectrum of trapped antiprotons is not a perfect match in all details with the in-situ observed flux spectra, we do note an excellent antiproton flux match around 1 GeV kinetic energy. Thus, we conclude that what we earlier had largely predicted, the Pamela antiproton detection experiment has now observed.

The unexpected rise of the positron to electron ratio with energy in the 20 ÷ 100 GeV range has been recently observed by PAMELA. Later, it was also confirmed by Fermi-LAT. In the last experiment it was additionally detected that the positron fraction continues to rise between 100 and 200 GeV. We report the results of new calculations of the positron to electron ratio in the wide energy range. Fractional diffusion model was implemented to describe the particles propagation from sources.

It is shown that a self-consistent description of the experimental data can be obtained if we assume that both positrons and electrons are injected into the interstellar medium by the sources with the same spectral exponent p ≈ 2.85. We have also found that the positron to electron ratio increases to a constant value of ~ 0.22 for energies E > 100 GeV. This flattening of the positron fraction obtained in our model for E > 100 GeV can be examined in the near future by the AMS-02 experiment.

In our previous papers we proposed an anomalous diffusion model for solution of the knee problem in the primary cosmic-rays spectrum and explanation of different values of spectral exponent of protons and other nuclei at wide energy region. The anomaly results from large free paths (Levy flights) of particles between magnetic domains. The physical arguments and the calculations indicate that the bulk of observed cosmic rays with energy 10⁸ – 10¹⁰ eV is formed by numerous distant (r > 1 kpc) sources. It means that the contribution of these sources to the observed flux may be evaluated in the framework of the steady-state approach (J_G). The contribution of the nearby (r < 1 kpc) relatively young (t < 10⁵ yrs) sources defines the spectrum in the high energy region and provides the knee (J_L). Consequently the cosmic rays intensity from all galactic sources for some group of nuclei consists of local J_L and global J_G components.

We show that in the framework of our anomalous diffusion model with two-component representation of CR intensity the behavior of proton to helium ratio observed by PAMELA can be reproduced.

A prototype of the PRISMA project array has been deployed and started running on the basis of the NEVOD complex at National Research Nuclear University MEPhI. It consists now of 32 detectors of a novel type (en-detector) sensitive to two main EAS components: electromagnetic (e) and hadronic (through thermal neutrons (n)) ones. The purpose of the array is testing and developing of a new experimental method of EAS study through neutron and electromagnetic components recording, optimization of the detector design and the data acquisition system. First experimental results are presented and compared with first Monte-Carlo simulations.

Recently, details of modular cosmic ray detectors developed by the staff of the SVIRCO Observatory and Terrestrial Physics Laboratory (Rome, National Institute for Astrophysics) were published (Signoretti and Storini, 2011). Data recorded during June 2011 by a modular mobile neutron detector, equipped with a large helium counter (5.08 cm in diameter, 191 cm long) and assembled with twenty-three modules, were carefully checked and used to investigate the detector response to the perturbations originating on the Sun and travelling through the interplanetary medium. We show that at the Rome rigidity threshold (about 6.3 GV) the registered intensity well accounts for the macro perturbations in the near-Earth Space. Nevertheless, to investigate the fine structure of the perturbations the modular detector should operate at mountain altitudes or in polar areas.

Traditional inspection methods are of limited use to detect the presence of fissile (U, Pu) samples inside containers. To overcome such limitations, prototypes of detection systems based on cosmic muon scattering from high-Z materials are being tested worldwide. This technique does not introduce additional radiation levels, and each event contributes to the tomographic image, since the scattering process is sensitive to the charge of the atomic nuclei being traversed. A new Project, started by the Muon Portal Collaboration, plans to build a large area muon detector able to reconstruct muon tracks with good spatial and angular resolution. Experimental tests of the individual detection modules are already in progress. The design and operational parameters of the muon portal under construction are here described, together with the preliminary simulation and test results. Due to the large acceptance of the detector for cosmic rays, coupled to the good angular reconstruction of the muon tracks, it is also planned to employ such detector for cosmic ray studies, complementing its detection capabilities with a set of trigger detectors located some distance apart, in order to measure multiple muon events associated to extensive air showers.

Results of the experimental research, performed within the framework of the OLIMPIYA project on investigation of the relict galactic cosmic ray nucleus tracks in olivine crystals from the Marjalahti and the Eagle Station meteorites, are presented. Up to now, there were processed 170 crystals, and about 6000 tracks with nuclear charge Z > 55 were registered. About 45 tracks are identified as nuclei with charge of 88 < Z < 92. Charges of three nuclei, associated with super long tracks, exceed Z = 92. In the first approximation the charge value of two of these nuclei lies in the range of 105 < Z < 130. The charge of one of them is estimated as Z = 119±6. We believe that confirm the hypothesis of the existence of "stability islands" for natural trans-Fermi nuclei.

New results concerned to the investigation of depth-dependent the pit-like surface-average and the grouping track-density distributions in the cosmic ray exposed column of CN-85 and CR-39 plastic solid state nuclear track detectors (SSNTD) are presented. Two main sources: solar cosmic ray protons and recoil nuclei for very short (length <3 μm) track-pit formation are considered. Theoretical estimation of the total, uniform track-pit density indicates on failure of evidence of some additional radiation effects, partially, hypothetically conditioned with the Erzion theory. Some quantitative proofs of this hypothesis have been obtained in the measurements of the pit-groups. Totally, up to this time it was registered near of 30 pit groups with the surface pit-density in the interval of (1-15) × 10⁶ cm², that is two-three orders of magnitude higher than uniformly distributed track-pits on the same CR-39 plate surface. As a result of layer-by-layer investigation of the exposed CN-85 stock arrangement three pit swarms exactly correlated with the end point of high ionizing primary charge particle tracks were observed. Obtained data are considered in according to submission based on the probability of detection for the negative charged cosmic ray Erzion particles stopping events.

Shower-by-shower fluctuations play a key role for the understanding of EAS morphology. Each observed event keeps track of the propagation through the atmosphere. This factor can influence the shape of time front and the sequence of arrival times. The design of the ARGO-YBJ detector offers a unique chance to have high resolution pictures of shower footprints at the ground. The time structure of the shower disc has been studied as a function of the distance to the shower axis. The curvature of the shower front, defined as the mean of time residuals with respect to a planar fit, has also been investigated in the energy range between 300 GeV and 100 TeV and its features employed to characterize the standard surface array observables. After a study on the shower time profile and on the lateral distribution at different time delay from the shower front, showers with large time residual rms with respect to the shower front have been investigated. The longitudinal time structures in data could help to better define selection criteria for particular analysis, such as gamma/hadron separation, composition or "exotic" physics, and allow a better determination of EAS disc structure and correlations between front profile, front thickness and core distance.

The anomalous diffusion model for cosmic rays transport in fractal-like galactic medium developed by the authors allows to describe main features of the observed spectrum of charged particles arriving in the Solar system. Anomalous diffusion equation underlying the model contains fractional derivative operators and do not take into account the finite speed of particles transport. In this regard, we conducted a Monte Carlo simulation of uncoupled continuous-time random walks of particles in this model. The particles can perform an anomalously large jumps between scattering centers (Levy flights) and also can stay a long time in the inhomogeneities of the medium (Levy traps). The probability of such behavior of particles is described by power-law distributions for the jumps length and for the residence time in the inhomogeneity. In this paper, we present the spatial distribution of particles obtained from the direct simulations of particle trajectories in the framework of our model for two versions: considering finite particle speed and the case of an instantaneous jump.

Results of four year cosmic ray anisotropy measurement, done with Baksan Carpet-2 array at the energy region 10-100 TeV, as a function of energy are presented. Data analysis was performed with "East minus West" method with subsequent Farley-Storey correction on anti-sidereal wave. The amplitude and phase of anisotropy for three integral energy ranges E > 17 TeV, E > 62 TeV and E > 100 TeV are reported.

Recent data from ATIC, CREAM and PAMELA revealed that the energy spectra of cosmic ray (CR) nuclei above 100 GeV/nucleon experience a remarkable hardening with increasing energy. This effect cannot be recovered by the conventional descriptions of CR acceleration and diffusive propagation processes. Using analytical calculations, I show that the hardening effect can be consequence of a spatial change of the CR diffusion properties in different regions of the Galaxy. I discuss the implications of this scenario for the main CR observables and its connections with the open issues of the CR physics.

The neutron monitor in Barentsburg is equipped with a modernized data acquisition system which allows registering time intervals between pulses with 1 μs accuracy. This high resolution makes it possible to study such fast and transient phenomenon like multiplicity. A multiplicity event is an isolated sequence of pulses with short time intervals between them. The Barentsburg neutron monitor consists of three sections, which are spaced at 5 m. In the present work a two-section multiplicity was studied, i.e. multiplicity events which are formed by pulses of two sections. We have assigned that each section must input no less than 4 pulses into an event to have a two-section multiplicity. The probability of a random coincidence of single pulses in this case is around 10–⁸ (one event per ~10 days). But the real number of such events is ~10 per day. The other characteristics of two-section multiplicity events (total time duration, time profile etc.) are similar to the values of one section multiplicity. So this is undoubtedly real multiplicity. We consider it to be an effect of atmospheric hadronic shower on the NM. The cross-section size of such shower is estimated about 10 m according to the distance between sections.

The flux of fast neutrons produced by CR muons in lead at the depth of 25 mwe is measured. Lead is a common shielding material and neutrons produced in it in muon interactions are unavoidable background component, even in sensitive deep underground experiments. A low background gamma spectrometer, equipped with high purity Ge detector in coincidence with muon detector is used for this purpose. Neutrons are identified by the structure at 692 KeV in the spectrum of delayed coincidences, caused by the neutron inelastic scattering on Ge-72 isotope. Preliminary result for the fast neutron rate is 3.1(5) × 10^−-4n/cm² · s.

Using data taken by the Pamela experiment during 5 years of operation we studied the anisotropy in the arrival direction of cosmic ray electrons and positrons with energy above 40 GeV. We report on a study of anisotropy in the e^± flux at different angular scales extending from 30° up to 90°, furthermore a directional analysis has been performed around the Sun direction. The observed distribution of arrival directions is consistent with the isotropic expectation at any angular scale used in this study and no significant evidence of strong anisotropies has been observed, also the analysis around the Sun direction did not show any significant excess.

The new method based on the classification algorithms was developed to separate antiprotons and electrons in the PAMELA experiment. Training samples based on Monte-Carlo simulation of particle's interactions in the PAMELA imaging Si/W calorimeter were used to achieve rejection factor and to keep high antiproton efficiency. With comparison to the previous publication the number of events was increased 1.5 times. Information collected from the mission start in 2006 till January 2010 was used in the analysis. 2800 events were found in the energy range from 60 MeV to 350 GeV. The flux of antiprotons in galactic cosmic radiation obtained with new method is presented.

Two models based on fractional differential equations for galactic cosmic ray diffusion are applied to the leaky-box approximation. One of them (Lagutin-Uchaikin, 2000) assumes a finite mean free path of cosmic ray particles, another one (Lagutin-Tyumentsev, 2004) uses distribution with infinite mean distance between collision with magnetic clouds, when the trajectories have form close to ballistic. Calculations demonstrate that involving boundary conditions is incompatible with spatial distributions given by the second model.

Size estimation is a challenging area in the field of Ultra High Energy (UHE) showers where actual measurements are always associated with uncertainty of events and imperfections in detection mechanisms. The subtle variations resulting out of such factors incorporate certain random behaviour in the readings provided by shower detectors for subsequent processing. Field strength recorded by radio detectors may also be affected by this statistical nature. Hence there is a necessity of development of a system which can remain immune to such random behaviour and provide resilient readings to subsequent stages. Here, we propose a system based on Artificial Neural Network (ANN) which accepts radio field strength recorded by radio detectors and provides estimates of shower sizes in the UHE region. The ANN in feed-forward form is trained with a range of shower events with which it can effectively handle the randomness observed in the detector reading due to imperfections in the experimental apparatus and related set-up.

Cosmic ray acceleration takes place in shocks of relativistic jets in Active Galactic Nuclei (AGN). The diffusive or stochastic acceleration are believed to be the main responsible mechanisms. Additionally, it is known that the back-reaction of accelerated cosmic rays in shock fronts in astrophysical environments, may lead to the formation of a precursor shock with a length scale which corresponds to the diffusive scale of the energetic particles. In this work we will investigate the properties of relativistic, parallel and perpendicular precursor shocks, via numerical test-particle simulations, allowing diffusive and stochastic acceleration.

The primary proton tracks are identified in about half of events referred to proton ones in the Russian-Japanese balloon-born emulsion chamber RUNJOB experiment. Reprocessing of experimental data obtained in long-term exposure of RUNJOB-3B, 6A, 11A, 11B emulsion chambers (EC) with new method for searching of the primary cosmic particles leads to confirm that as well as earlier single charged primary tracks are not found in about half of events referred to the proton ones with energy E₀> 20 TeV and zenith angle tg(θ) ≤ 5. In this paper the new method for searching and tracing of the primary cosmic particles in EC's and characteristics of studied events (energy, angle, pass length of the primary particles until their interaction in EC) are presented.

A dose rate data on different spacecrafts at circular orbit ~20000km were obtained, also a comparison between the flight data and space models was made and anomalous perturbations of ionizing radiation of spacecrafts was traced. These abnormal disturbances are correlated with GOES data and with International Space Station data, and also with ground based measurements of neutron monitors.

One of the elements of industrial system of monitoring is a local ground forecast station, which provides forecasts of geophysical conditions, including the forecast of the proton increase, geomagnetic forecasts, forecasts of relativistic electrons, and produces an alert signal when protons and electrons increase.

In this paper, a probable interpretation of a remarkable fine structure of all particle spectra between the knee and the ankle, as well as a high content of heavy nuclei around 10¹⁷ eV measured recently in Tunka-133 and KASCADE Grande experiments, is presented: the special class of sources, SN_Ia, provides cosmic rays (CR) around the knee. Subtracting the contribution of them from all particle spectrum we obtained the residual flux of the CR corresponding to the transition region between Galactic and Extragalactic CR in the range 10¹⁷ ÷ 5 10¹⁸ eV. The obtained spectrum also has a pronounced knee at energy (2÷3)10¹⁷ eV and slopes γ₁ ~ 1.8+0.3 before it and γ₂ ~3.4 above it. We analyzed the possible contribution from known Galactic sources and shown that formally the best candidate to contribute significantly to the transition region is Cas A. This source posses a number of unusual properties and considered as Type IIb SNR. However we show that the hypothesis of extragalactic CR origin providing the region above 10¹⁷ eV seems to be more realistic.

Different lateral and energetic characteristics of gamma-ray families produced in nucleus-nucleus (AA) interactions of primary cosmic rays (PCR) are studied. Primary mass composition analysis performed on the basis of "Pamir" Collaboration X-ray emulsion chambers (XREC) data by using of selection criteria of gamma-ray families originating from AA-interactions above 10 PeV. Experimental data are compared with results of MC0 algorithm based on quark-gluon string model (QGSM). Among seven considered variables, only two lateral parameters, R_1E and ρ, are not described by the MC0 model.

Solution of the problem of proton acceleration in Gamma-Ray Bursts is suggested. The acceleration occurs in the relativistic shocks via the surfatron mechanism (surfing). It is shown that the proton acceleration up to 10¹⁴ – 10¹⁷ eV is possible in the case of a spherical shock (fireball); the flat shock accelerates up to 10¹⁶ – 10²⁰ eV.

Propagation of ultra-high energy nuclei in expending universe filled with background radiation is considered. We developed numerical code for solution of inverse problem for cosmic-ray transport equation that allows determination of source spectrum from the spectrum observed at the Earth. The injection spectra of protons and iron nuclei in extragalactic sources are found assuming that these species dominate in the source composition. Data from the Auger and Telescope Array experiments are used to illustrate the method.

The analysis of experimental data from the Tien Shan complex array on extensive air showers originated from 0.5-5 PeV primary cosmic rays is presented. Conclusions are made on the rise of the inelastic proton–air cross section with energy on the base of comparisons with different interaction models. The analysis showed that the rise conforms to (7-9) % per one order of energy from 0.2 TeV (accelerator experiments with fixed targets) to 5 PeV (cosmic rays). These data correspond better to the new QGSJET-II-04 version of the interaction model based on the recent LHC results. This model predicts the slower rise of the cross-section than previous versions of QGSJET-II models.

EMMA (Experiment with MultiMuon Array) is a new approach to study the composition of cosmic rays at the knee region (1 – 10 PeV). The array will measure the multiplicity and lateral distribution of the high-energy muon component of an air shower and its arrival direction on an event-by-event basis. The array operates in the Pyhäsalmi Mine, Finland, at a depth of 75 metres (or 210 m.w.e) corresponding to the cut-off energy of approximately 50 GeV for vertical muons. The data recording with a partial array has started and preliminary results of the first test runs are presented.

The composition of the primary cosmic radiation should be studied by various alternative approaches. A promising way is to exploit a dependence of the fraction of muons in an extensive air shower on the atomic number of the primary nuclei. A comparison of the fraction of muons at 600 m from the shower axis observed at the Yakutsk array in the vertical air showers at ultra-high energies with results of simulations in terms of QGSJET-II and Gheisha-2002d models carried out with the help of the CORSIKA 6.616 and GEANT4 codes showed rather heavy composition of the primary radiation. But some errors in these models should be taken into account. At last, one has to allow for the fact that signals in the surface and underground scintillation detectors of the Yakutsk array from various particles of extensive air showers are measured in different units. All these corrections taken together show the proton composition of the primary radiation in the energy region of ~2.·10¹⁸ – 10¹⁹ eV. At lower energies a composition is heavier. The change from the heavy composition to the primary protons occurs in the energy interval of 9.·10¹⁷ – 2.·10¹⁸ eV. It is not excluded that at energies above 1.1·10¹⁹ eV the composition may be also heavier as illustrated by a trend of data.

Yakutsk extensive air shower array experiment is the only one which is in operation since 1974, it has the best exposure around 10¹⁸eV. It is believed that the balk of cosmic rays up to ~10¹⁷eV originated in supernova remnants [1]. Under certain conditions they can accelerate cosmic rays up to ~10¹⁸eV or even higher [2]. However, there is a lack of an undoubted observational evidence for such idea. Here we show that Yakutsk experiment probably has observed cosmic rays from SN 1987A. We found that before 1996 the intensity of cosmic rays in energy range 10^17–10¹⁸eV fluctuate near some average value, then it start to increase. The increase of intensity total 45±5%. It is also accompanied by significant changes in cosmic ray composition; it became heavier – iron dominated. In the last 3-4 years it is a trend to return to the initial state. This peculiarities can be explained by the appearance of SN 1987A. If so, then our results demonstrate that supernova remnants can indeed accelerate cosmic rays up to ~10¹⁸e V. This is an important step in understanding the cosmic ray origin problem and reveal the great importance of long-term and multicomponent observations of ultra-high energy cosmic rays.

Results of radio emission measurements at 30-34 MHz from extensive air shower particles with primary energy above 10¹⁷ eV are presented. The data recorded at the Yakutsk EAS for the period 2009 – 2011 years with energies above 10¹⁷ eV, zenith angles less than 60 degree, the axes of which were within a large EAS. The shape of the spatial distribution has a different slope, depending on the distance to the shower axis. At large distances R > 500 m from the shower radio emission is small and almost constant up to a distance of 800 m. The primary energy of EAS and the amplitude of the peak radio pulse are correlated.

Distribution of maximum depths of extensive air showers (EAS) with energies of 10¹⁷–10¹⁸ eV is restored from the lateral distribution of EAS radio emission measured by the LOPES experiment (40-80 MHz). Dependence of the EAS maximum depth on its energy is constructed and mass composition of cosmic rays is estimated. It follows from the obtained dependencies that the fraction of light cosmic ray's nuclei increases in the energy range under consideration.

Usually it is supposed that the definition of the CR mass composition in knee region is the key to problem of CR spectrum modification in this range. However tens of experiments done for the last half a century, have not decided this problem. The possible causes of fiasco and arguments in favour of necessity to reformulate a method of attack are discussed. It is formulated that the first experimental task now is to solve a more simple problem: is there abnormal CR component in knee field or not. It seams that impossible to formulate correctly more common problem of mass composition without solving of this one. The observational basis is discussed. The hypothesis of strange quark matter is suggested for the abnormal component.

The Auger Engineering Radio Array (AERA) is designed to study the radio emissions from extensive air showers at the Pierre Auger Observatory. The array currently consists of a grid of 23 autonomous radio detector stations that measure the radio emissions from cosmic-ray-induced air showers since April 2011. The array is still under construction and is planned to be extended to 160 stations. The new detection technique provides an augmentation of the existing detectors, improves the sensitivity of the observatory and sheds new light on the shower physics. An analysis of the emission processes based on the polarization of the radio pulses is presented.

Dedicated to the measurement of the radio transients coming from the extensive air showers (EAS), the CODALEMA experiment was started in 2001 at the Nançay Observatory, in France. Benefiting of an easy deployment and a low cost compared with Cherenkov detectors or fluorescence telescopes, this alternative method appears to be an interesting tool for the understanding of the physics of high energy cosmic rays observed through EAS. A new configuration of the CODALEMA experiment was implemented in 2011 based on a standalone detection, which will be essential for the next generation of giant detector array. One of the major challenges of this promising detection mode is the control (identification and rejection) of the fluctuating and transient noise events in an inhabited area and the knowledge of the shower radio-detection capabilities such as the effective efficiency and the data purity. Some results concerning this new setup of the experiment will be discussed in this paper.

LOPES is a digital antenna array for the radio measurement of cosmic-ray air showers at energies around 10¹⁷ eV. It is triggered by the KASCADE-Grande air-shower array at the Karlsruhe Institute of Technology (KIT), Germany. Because of an absolute amplitude calibration and a sophisticated data analysis, LOPES can test models for the radio emission to an up-to-now unachieved level, thus improving our understanding of the radio emission mechanisms. Recent REAS simulations of the air-shower radio emission come closer to the measurements than any previously tested simulations. We have determined the radio-reconstruction precision of interesting air-shower parameters by comparing LOPES reconstructions to both REAS simulations and KASCADE-Grande measurements, and present our latest results for the angular resolution, the energy and the X_max reconstruction based on the radio measurement of about 500 air showers. Although the precision of LOPES is limited by the high level of anthropogenic noise at KIT, it opens a promising perspective for next-generation radio arrays in regions with a lower ambient noise level.

Tunka-Rex, the Tunka radio extension, is an array of about 20 antennas currently under construction, which covers an area of 1 km². Tunka-Rex measures the radio emission of cosmic-ray air showers above 10¹⁶ eV. It is triggered by the photomultipliers of the Tunka-133 experiment which simultaneously measure the Cherenkov light emitted by the same air showers. The radio-Cherenkov-hybrid measurements thus offer a unique opportunity for a cross-calibration of both detection methods. The main goal of Tunka-Rex is to determine the precision of the radio reconstruction for the energy and the atmospheric depth of the shower maximum, X_max, and thus to experimentally test theoretical predictions that the radio precision can be similar to the precision of air-Cherenkov and fluorescence measurements. At the same time, Tunka-Rex can demonstrate that radio measurements can be performed on a large area for a relatively cheap price, since the antennas will be connected to the already existing Tunka DAQ. Finally, radio-antenna arrays have the perspective to increase the effective observation time compared to air-Cherenkov and fluorescence detectors by an order of magnitude, since radio measurements are possible under almost any atmospheric and light conditions.

Using the data of the EAS MSU array and model calculations we have performed the search of events with abnormally small fraction of muons with energy above 10 GeV in showers with particle numbers greater than 2.10⁷ and with zenith angles less than 30 degrees. The aim of the work – to estimate a fraction of muon-poor showers in which the underground muon detector registered no muons. These events may be identified as showers generated by primary gamma-quanta of ultrahigh energies. With good statistical accuracy we have confirmed our earlier conclusion that the content of gamma-quanta in the primary cosmic ray flux may be as much as 2 % at energies about 10¹⁷ eV.

Double extensive air showers were investigated at Tien-Shan high mountain scientific station of P.N. Lebedev Institute by means of two various installations. One installation registered electron-photon air shower component, another – Vavilov-Cherenkov radiation. On both installations the double showers divided by a time interval of ~100 nanoseconds have been registered. In the present work frequency of occurrence of such showers in each of installations is analysed, and is shown that at supervision of vertical showers (zenith angle θ <60°) these frequencies coincide.

Data on most energetic particles in EAS cores (γ-ray-hadron families) obtained with XRECs at superhigh energies in stratospheric and high-mountain experiments are discussed. Transverse size and alignment of most energetic subcores in γ-h families are considered. Lateral features of γ-ray families are shown to be dependent on pt(x_Lab) at 0.05 x_Lab 0.20 in h-A interactions. Features of interactions at E₀ 10¹⁵ are formulated.

It is shown that recent experimental data in the knee region contradict each other and new approaches to the so – called "knee problem" are needed to solve this complicated and old problem. The PRISMA project proposed by us is based on an idea that the main EAS component – hadrons have to be measured first of all. Special detectors have been developed for this purpose. It is shown using Monte-Carlo simulations that only full-scale recording of hadronic component could give us a key to the solution. The location of such experiment should be at high altitude (the higher, the better) and that is why we proposed to combine the central part of the PRISMA array with that of the LHAASO project array to be constructed in Tibet. If the proposal will have success then the "knee problem" will be solved in a few years.

All-particle energy spectrum in the knee region obtained from extensive air shower (EAS) measurements (GAMMA experiment, 700 g/cm², Armenia) is presented. Energies of primary particles in the range of 10^6–10⁸ GeV were evaluated on the basis of observed shower parameters N_ch,N_μ, s, θ and corresponding parameterisation of CORSIKA simulated database for SIBYLL interaction model. All shower detection and reconstruction uncertainties were included in the simulated showers for four kinds (H, He, O, Fe) of primary nuclei. The reliability of observed all-particle energy spectrum is investigated from viewpoint of methodical errors and statistical fluctuations. Observed fine structure of all-particle energy spectrum can be interpreted by the rigidity-dependent steepening Galactic diffuse nuclei flux and an additional iron component in the region of 70-80 PeV primary energies most likely originated from nearby pulsars.

The Air Microwave Yield (AMY) project aims to measure the emission in the GHz regime from test-beam induced air-shower. The experiment is using the Beam Test Facility (BTF) of the Frascati INFN National Laboratories in Italy. The final purpose is to characterize a process to be used in a next generation of ultra-high energy cosmic rays (UHECRs) detectors. We describe the experimental apparatus and the first test performed in November 2011.

There are several instruments at the Yakutsk EAS array which are used for monitoring of atmospheric conditions. Here we present the results of perennial observations of the atmospheric spectral transparency, seasonal variations of aerosol optical depth, stratospheric temperature and ground-level electric field. These characteristics are used during the processing of primary data obtained by the EAS array.

The Yakutsk array group is developing the wide FOV Cherenkov telescopes to be operated in coincidence with the surface detectors of the array under modernization. Currently the engineering prototype of the reflecting telescope with front-end electronics is designed and assembled to prove the feasibility of the concept. In this report the status and parameters of the engineering prototype are presented.

The GELATICA experiment in Georgia (GEorgian Large-area Angle and TIme Coincidence Array) is devoted both to the Cosmic Ray (CR) energy spectrum investigation at very high energies and possible correlations in the arrival times and directions of separate Extensive Air Showers (EAS) over large distances. The timing distributions between the consecutive EAS events observed at the remote installations in the towns of Tbilisi and Telavi are considered. The expectation time for a consecutive pair of remote random EAS events at these two installations is estimated under the condition of their timing separation being less then a tolerable propagation time of shower front between the observation points.

The first measurements of the Experiment with MultiMuon Array (EMMA) have been analyzed for the selection of the Extensive Air Showers (EAS). Test data were recorded with an underground muon tracking station and a satellite station separated laterally by 10 metres. Events with tracks distributed over all of the tracking detector area and even extending over to the satellite station are identified as EAS. The recorded multiplicity spectrum of the events is in general agreement with CORSIKA EAS simulation and demonstrates the array's capability of EAS detection.

We search for ultra-high energy photons by analyzing geometrical properties of shower fronts of events registered by the Telescope Array surface detector. By making use of an event-by-event statistical method, we derive upper limits on the absolute flux of primary photons with energies above 10¹⁹ eV, 10^19.5 eV and above 10²⁰ eV based on the three years data from Telescope Array surface detector (May 2008 – May 2011). We report the results of down-going neutrino search based on the analysis of very inclined events.

First preliminary results of the balloon-borne experiment SPHERE-2 on the all-nuclei primary cosmic rays (PCR) spectrum and primary composition are presented. The primary spectrum in the energy range 10¹⁶–5 · 10¹⁷ eV was reconstructed using characteristics of Vavilov-Cherenkov radiation of extensive air showers (EAS), reflected from a snow surface. Several sources of systematic uncertainties of the spectrum were analysed. A method for separation of the primary nuclei' groups based on the lateral distribution function' (LDF) steepness parameter is presented. Preliminary estimate of the mean light nuclei' fraction f_30-150 at energies 3 · 10¹⁶–1.5 · 10¹⁷ eV was performed and yielded f_30-150 = (21±11) %.

The problem of PCR Composition at super high energies is far from being solved. EAS Cherenkov light spatial-angular distribution (CL SAD) can yield important information on the primary mass. In order to use EAS CL SAD for the study of PCR composition one needs a set of imaging telescopes with the appropriate parameters. On the basis of full Monte-Carlo simulations the main features of such telescopes are analyzed for a specific observation level 4km which is typical for the Eastern Pamir mountains.

An analysis was performed on a set of EAS events containing recorded pulses in scintillation detectors of various area and located at different core distances. Events were categorised by the energy and zenith angle. A difference in pulse shapes was noted between young and old showers. In the data bank, several events were highlighted, with identical delayed pulses recorded in one or more scintillation detectors. Involving multi-component analysis of extensive air shower data we discuss possible connection of a second shower front (which the delayed pulses effectively represent) with yet unknown processes.

Microwave radiation from extensive air showers is expected to provide a new technique to observe UHECR. We developed three set of radio telescopes in Osaka, in Kobe and at Telescope Array site in Utah, USA. In Osaka, we are coincidentally operating two Ku band radio telescopes with an air shower array which consists of nine plastic scintillators with about 10 m separation. In Kobe, we have started the operation of twelve radio telescopes of 1.2 m diameter in March 2012. In Utah, we installed two telescopes just beside the Black Rock Mesa fluorescence detector (FD) station of the Telescope Array experiment, and we operated the radio telescopes coincidentally with FD event triggers. We report the experimental setups and the results of these measurements.

Scaling properties of nuclei- and photon-initiated air showers are examined in wide primary energy range (10¹⁴ ÷ 10²² eV) taking into account Landau-Pomeranchuk-Migdal and geomagnetic field effects. It is shown that the invariance in lateral distribution and also the universal dependence between shower age and root mean square radius of electron component exist up to the highest energies. The implications of shower universality for reanalysis, crosschecking and validation of the results of different experiments together with decreasing of the influence of hadronic model uncertainties are discussed in detail.

Signals in the surface and underground scintillation detectors from the extensive air shower particles at the Yakutsk array are measured in some practical units. These units are signals in detectors caused by the near vertical muons. These signals from the near vertical muons in the surface and underground detectors have been simulated with the help of the GEANT4 package. These simulations follow up the real experimental calibration of the surface and underground detectors carried out at the Yakutsk array. Results of simulations show the noticeable difference of ~5% in energies deposited in these two types of detectors. This difference should be taken into account to interpret correctly data on the fraction of muons observed at the Yakutsk array and to make real conclusions about the composition of the primary cosmic radiation at ultra-high energies.

Here is presented the current state of the SPHERE-2 balloon-borne experiment. The detector is elevated up to 1 km above the snow surface and registers the reflected Vavilov-Cherenkov radiation from extensive air showers. This method has good sensitivity to the mass-composition of the primary cosmic rays due to its high resolution near the shower axis. The detector consists of a 1500 mm spherical mirror with a 109 PMT cluster in its focus. The electronics record a signal pulse profile in each PMT. In the last 2 years the detector was upgraded: time resolution of pulse registration was enhanced up to 12.5 ns, channel sensitivity was increased by a factor of 3, a new LED-based relative PMT calibration method was introduced, and new hardware and etc. was installed.

KASCADE-Grande is an air-shower observatory devoted to the study of cosmic rays with energies in the range 10¹⁶ – 10¹⁸ eV. In KASCADE-Grande, different detector systems allow independent measurements of the number of muons (N_μ) and charged particles (N_ch) of air showers, which are the basis for several energy and composition studies of cosmic rays. In this contribution, a composition analysis using the shower size ratio lgN_μ/lgN_ch, corrected for attenuation in the atmosphere, is described. Using QGSJET II-based simulations of different primaries, it is shown that an energy independent cut on the shower ratio can be chosen in order to separate the cosmic ray events into light and heavy mass groups. The analysis is applied to the KASCADE-Grande data. The energy spectra derived from the analysis are presented.

The problem of detecting cosmic rays and neutrinos of energies above the GZK cutoff is reviewed. Nowadays, it becomes clear that registration of nature's most energetic particles requires approaches based on new principles. First of all, we imply the detection of the coherent Cherenkov radio emission in cascades of ultrahigh-energy particles in radio-transparent natural dense media, i.e., ice shields of Antarctica, mineral salt, and lunar regolith. The Luna-Glob space mission planned for launching in the near future involves the Lunar Orbital Radio Detector (LORD) whose aperture for cosmic rays and neutrinos of energies E ≥ 10²⁰ eV exceeds all existing ground-based arrays. The feasibility of LORD to detect radio signals from showers initiated by ultrahigh-energy particles interacting with the lunar regolith is examined. The design of the LORD space instrument and its scientific potentialities for registration of low-intense cosmic-ray particle fluxes above the GZK cut-off up to 10²⁵ eV is discussed.

The Telescope Array experiment is the largest hybrid detector to observe Ultra-High Energy Cosmic Rays in the northern hemisphere. The observation started in November 2007 for Fluorescence Detector (FD) and in March 2008 for Surface Detectors (SD). Here, we present the preliminary results of the energy spectrum and mass composition of the UHECRs measured by the FD and hybrid technique from the Telescope Array three year observations. The energy spectrum measured by the Middle Drum FD station, which is the refurbished HiRes-I detector is consistent with the results from HiRes. The energy spectrum with the two newly constructed FDs and SD is also in good agreement with the result from HiRes, especially for the energy scale. The mass composition study with the slant depth of the maximum shower development (X_max) is obtained by using the stereo and hybrid analysis. The result of the mass composition is consistent with the proton prediction.

New setup for detection of EAS electromagnetic component at the knee region of primary energies is under construction on the basis of the experimental complex NEVOD (Moscow, Russia). The measuring system of the EAS array has a cluster organization. Clusters are located on the roofs of laboratory buildings of MEPhI (Moscow). Features of measuring and DAQ systems, results of investigations of characteristics of a single counter and the event formation algorithm from the data of separate clusters are discussed.

This paper analyses mass composition of high-energy cosmic ray, comparing simulation and experimental results. Using the nuclear interaction models QGSJET-II and Sibyll, we simulate EAS initiated by the primary nuclei representing all mass groups (p, He, O, Si, Fe). EAS is simulated for several energy levels between 1.10¹⁸ and 5.10¹⁹ eV. For such generated simulation data, we compute X-max distributions, mean X-max and RMS and compare these values with the experimental data from the Auger Experiment. The results show that for the 2-sigma confidence level, mass composition including nuclei from the CNO group and heavier can be fitted for Sibyll model only. For any combination of 3 and 4 primary particles, no model fits the experimental data at the 1-sigma confidence level. For the p + Fe bi-particle composition, or other combination of two particles, also no model fitting the experimental data can be found for the analysed energy interval.

The origin of ultra-high-energy cosmic rays (UHECRs) is one of the most intriguing problems of modern cosmic ray physics. We briefly review the main astrophysical models of their origin and the forthcoming orbital experiments TUS and JEM-EUSO, and discuss how the new data can help one solve the long-standing puzzle.

KASCADE-Grande is a large detector array for observations of the energy spectrum as well as the chemical composition of cosmic ray air showers up to primary energies of 1 EeV. The multi-detector arrangement allows to measure the electromagnetic and muonic components for individual air showers. In this analysis, the reconstruction of the all-particle energy spectrum is based on the size spectra of the charged particle component. The energy is calibrated by using Monte Carlo simulations performed with CORSIKA and high-energy interaction models QGSJet, EPOS and SIBYLL. In all cases FLUKA has been used as low-energy interaction model. In this contribution the resulting spectra by means of different hadronic interaction models will be compared and discussed.

We review the observations of Ultra High Energy Cosmic Rays (UHECR), focusing on the energy spectra as measured by HiRes, Telescope Array (TA) and Auger detectors. We found that highest energy Auger steepening does not agree with GZK cutoff, which is most probably explained by the nuclei mass composition detected by Auger. At present the difference in mass composition in Auger and HiRes/TA data remains the main unsolved problem of UHECR origin.

In many UHECR experiments, some excess of muons is observed, which cannot be explained in frame of the existing theoretical models of hadron interaction. Attempts of its explanation through a heavy mass composition of PCR contradict the results of X_max measurements. Really, the excess of muons appears already at lower energies (10¹⁶ − 10¹⁷ eV), but in this domain it may be explained by the trend to a heavier mass composition, which is in a qualitative agreement with the galactic model of CR origin. The absence of heavy nuclei at energies of the order of 10¹⁸ eV requires to consider other possibilities of the appearance of muon excess, including changes of hadron interaction model. The actuality of the considered problem is connected with plans of future experiments in UHECR physics, in which the necessity of its solution must be taken into account.

With the forthcoming of space borne observatories devoted to research Ultra High Energy Cosmic Rays (UHECR) in the decade of 10²⁰eV, new challenges are posed to the experimental techniques. Mounted on the International Space Station, the Extreme Universe Space Observatory on board the Japanese Experimental Module (JEM-EUSO) will rely on the well established fluorescence technique to observe Extensive Air Showers(EAS) propagating in the atmosphere from space. The EUSO Simulation and Analysis Framework (ESAF) has been developed in this context to provide a full end-to-end simulation frame. Within ESAF the angular reconstruction modules rely on an a priori knowledge of the photoelectrons that were produced by an EAS and were also detected by the focal surface. Therefore, there is the need for a tool that discriminates between EAS-photoelectrons and background. In this paper we discuss the Peak and WIndow SEarching (PWISE) technique, which we have implemented inside ESAF as a module to perform the discrimination of the EAS photoelectrons. This is essential since the angular reconstruction modules rely on the knowledge of the EAS-photoelectrons. We also present some first results of the angular reconstruction using this module within ESAF.

The TUS orbital experiment is aimed to study energy spectrum, composition and arrival directions of the Ultra High Energy Cosmic Rays (UHECR) at E ~ 10²⁰ eV. The TUS mission is planned for operation at the dedicated "Mikhail Lomonosov" satellite. The TUS detector will measure the fluorescence and Cherenkov light radiated by EAS of the UHECR using the optical system – Fresnel mirror-concentrator of 7 modules of ~2 m² area in total. Status of the Fresnel mirror production, its optical parameters measurement and the TUS trigger system simulation are presented.

The JEM-EUSO instrument is a wide-angle refractive telescope in near-ultraviolet wavelength region being proposed for attachment to the Japanese Experiment Module onboard ISS. The instrument will study the fluorescence light produced in atmosphere by UHECR of energy E > 5 10¹⁹ eV. It consists of high transmittance optical Fresnel lenses with a diameter of 2.5 m, a focal surface covered by 4932 MAPMTs of 64 pixels, front-end readout, trigger and system electronics. The tracks generated by the Extensive Air Showers produced by UHE primaries propagating in the atmosphere, are reconstructed on the focal surface by registering in a cyclic memory, every 2.5 microseconds, the data coming from the 315648 pixels and by selectively retrieving only the interesting ones on the occurrence of a second level trigger. In order to guarantee the correct time alignment of the events and to measure the arrival time of the event with a precision of few microseconds, a clock distribution and time synchronization system for the focal surface electronics has been developed. In this poster we will present the status and the technical solutions adopted so far. We will also discuss the Data Processor of EUSO-BALLOON experiment, the JEM EUSO pathfinder mission, in which a telescope of smaller dimension respect to the one designed for the ISS, will be mounted on board a stratospheric balloon. The main objective of this pathfinder mission, planned for the 2013, is to perform a full scale end-to-end test of all the key technologies and instrumentation of JEM- EUSO detectors. Furthermore EUSO-BALLOON will measure the atmospheric and terrestrial UV background components, in different observational modes, fundamental for the development of the simulations.

We present evidence from the Pierre Auger Observatory that the models currently used in simulation of cosmic ray air showers at the highest energies predict less muons than observed in data in the energy range around 10¹⁹ eV. We explain the different methods used to estimate the number of muons, apply them to observations, and compare the results to predictions from simulations of air showers. The number of muons in EAS derived from the observations of the Pierre Auger Observatory is a factor of 1.5 to 2.2 higher than that predicted in simulations. The exact discrepancy depends on the zenith angle and, to a lesser extent, on the hadronic interaction model and analysis technique.

We report recent results from the Pierre Auger Observatory about the study of the anisotropy in the arrival directions of ultra-high energy cosmic rays. We present the results of the search for a dipolar anisotropy at the EeV energy scale. Measurements of the phase and the amplitude of the first harmonic modulation in the right-ascension distribution are discussed. For cosmic rays with energies above 55 EeV, we present an update of the search for correlations between their arrival directions and the positions of active galactic nuclei from the Véron-Cetty and Véron catalog. We also discuss the results of correlation analyses applied to other populations of extragalactic objects. Finally we present the search for anisotropies in the data without the usage of astronomical catalogues.

Lateral divergence of most energetic particles in EAS cores (γ-ray families) are shown to be independent of secondary particles' (p_t) in h-A interactions, but strongly determined by p_t(x_L) dependence at 0.05 x_L 0.30. Average x_L- and x²_L-weighted p_t-dependent parameters calculated in "truncated" x_L intervals are proposed to characterize interaction model features related to the lateral dimension of γ-ray families.

We present the results of observations of two types of Galactic supernova remnants with the SHALON mirror Cherenkov telescope of Tien-Shan high-mountain Observatory: the shell-type supernova remnants Tycho, Cas A and IC 443; plerions Crab Nebula, 3c58(SN1181) and Geminga (probably plerion). The experimental data have confirmed the prediction of the theory about the hadronic generation mechanism of very high energy (800 GeV − 100 TeV) gamma-rays in Tycho's supernova remnant. The data obtained suggest that the very high energy gamma-ray emission in the objects being discussed is different in origin.

Galaxy NGC 1275 is the central dominant galaxy of the Perseus Cluster of Galaxies and is of Seyfert galaxy class. NGC 1275 is known as powerful X-ray and radio source. In 1996 year a new metagalactic source was detected by SHALON at TeV energies. This object was identified with Seyfert galaxy NGC1275. The image and spectral energy distribution of NGC 1275 as well as 3c382 are presented. The recent detection by the Fermi LAT of gamma-rays from the NGC1275 makes the observation of the energy E > 100 GeV part of its broadband spectrum particularly interesting. The available high and very high energy data for NGC 1275 are well fitted in this model with three components.

The BL Lac objects come in two subclasses: the "low-frequency-peaked BL Lac objects" in which the synchrotron peak falls in the IR-optical range and the "high-frequency-peaked BL Lac objects" where it falls in the UV-X-ray bands. The observation results of high-frequency peaked BL Lac object: Mkn421 (z = 0.031), Mkn501 (z = 0.034), Mkn 180 (z = 0.045) and low-frequency peaked BL Lac object OJ 287 (z=0.306) are presented with integral spectra, images and spectral energy distributions combined with those in all broad energy range. Mkn 180 and OJ 287 blazars were recently detected by SHALON Cherenkov telescopic system.

Extragalactic background radiation blocks the propagation of TeV gamma-ray over large distances by producing e⁺e⁻ pairs. As a result, primary spectrum of gamma-source is changed, depending on spectrum of background light. So, hard spectra of Active Galactic Nuclei with high red shifts allow the determination of a EBL spectrum. The redshifts of SHALON TeV gamma-ray sources range from 0.018 to 1.375 those spectra are resolved at the energies from 800 GeV to about 50 TeV. Spectral energy distribution of EBL constrained from observations of Mkn421, Mkn501, Mkn180, OJ287, 3c454.3 and 1739+522 together with models and measurements are presented.

Recent experiments with satellite gamma-ray telescopes Fermi-LAT and AGILE in which bursts of gamma-rays from the Crab Nebula were detected in the energy range around 100 MeV have aroused keen interest, if not sensation. However, as long ago as more than 20 years from now the data on a possible burst in the Crab Nebula at much higher energies, about 100 TeV, were published. Characteristics of transient and stationary fluxes of gamma rays from the Crab Nebula in various energy ranges are discussed in this paper, and it is shown that the old data obtained at ultra-high energy can be reasonably consistent with the modern pattern of burst activity of the source.

The Pierre Auger Observatory is a hybrid detector of Ultra High Energy Cosmic Rays (UHECRs) especially suitable for primary energies above 10¹⁸ eV. Auger is also sensitive to primary neutral particles, namely photons, neutrinos and neutrons. Neutral cosmic rays propagate along a straight line and are not deflected by magnetic fields, in contrast to charged cosmic rays. This opens the possibility of doing "astronomy" by directional pointing. The most accepted astrophysical models predict the production of neutral particles both in their sources or in physical processes during the propagation of charged particles. We perform independent analyses for different types of neutral particles. No significant evidence of the presence of these particles has been observed in data collected from 2004 up to now; therefore we present upper bounds to their fluxes.

Supernova remnants are a probable site of acceleration of particles via diffusive shock processes. High energies carried by electrons or protons are radiated into photons detectable from radio to γ rays. MAGIC has recently observed W51C, one of the most luminous galactic supernova remnants, and completed its spectrum between 50 GeV and 5 TeV. We modelled different processes for high energy photon emission of this source, and compared the predictions with the measured spectral energy distribution. It is plausible that hadrons are accelerated in the expansion front of this source, in interaction with the surrounding molecular cloud, and photons are produced in the decay of neutral mesons created in hadronic collisions.

The formation and evolution of superdense clumps of dark matter (DM) is studied. DM clumps (DMC) can be observed via gamma-radiation from DM particles annihilations. Annihilation signal from the dark matter could be greatly increased due to the small-scale clumpiness. It provides the additional possibilities for the indirect DM particle identification. The superdense DMCs can be produced from the spiky features in the spectrum of inflationary perturbations or around cosmic strings loops. Being produced very early during the radiation-dominated epoch, superdense DMCs evolve as isolated objects. They do not belong to hierarchical structures for a long time after production, and therefore they are not destroyed by tidal interactions during the formation of larger structures. Superdense DMC can also be observed by by the gravitational wave detectors.

Most part of gamma-ray bursts (GRBs) spectra are well described by Band model with following parameters: α, β (spectral indices in low and high energy bands) and E_peak (energy of spectral peak). For several GRB parameter β characterizing the spectral shape in the region up to some hundred MeV (for example, GRB100724B). Moreover, Band spectrum of GRB080916C covering 6 orders of magnitude. Until recently spectral hardness parameter H₃₂ (the ratio of total counts in the 100 − 300 keV and 50 − 100 keV energy range) was used for additional classification events on hard and soft, for GRBs groups selection on hardness and duration distributions (subgroup of intermediate bursts) and so on. However, H₃₂ is defined in energy intervals 50−100 keV and 100−300 keV, but for some GRB E_peak> 300 keV and this value is outside regions of H₃₂ definition. Thus, parameter H₃₂ is incompletely represents spectral properties of such events. Basing on Band model we introduce new integral criteria could be used in the wide energy band for data analysis in past experiments such as BATSE (0.02 − 2 MeV), COMPTEL (0.8 − 30 MeV); EGRET (20 MeV − 30 GeV); in now operated experiments Fermi (8 keV − 1MeV, 200 keV − 40 MeV and 300 MeV − 300 GeV), AGILE (18 − 60 keV and 30 MeV − 50 GeV) and in future experiments: GAMMA−400 (0.1 − 3000 GeV) and so on. In the present work spectral parameters taken from BATSE and from Fermi catalogues were analyzed and the new integral criteria were investigated. Results of data studying have shown that new criteria allow making GRB classification including intermediate bursts subgroup separation.

With the HiSCORE (Hundred*i Square kilometer Cosmic ORigin Explorer) experiment we aim at the exploration of the accelerator sky using indirect air shower observations of cosmic rays from 100 TeV to 1 EeV and gamma rays above 10 TeV to several PeV. In this paper the HiSCORE detector is discribed and the results of the first prototype deployment are shown. Several components are discussed like the photomultiplier tubes, the clip-sum-trigger and the DRS4 based data acquisition. We present data taken with a first prototype station in April 2012 at Tunka.

The HiSCORE (Hundred*i Square-km Cosmic ORigin Explorer) detector aims at the exploration of the accelerator sky, using indirect air-shower observations of cosmic rays from 100 TeV to 1 EeV and gamma rays in the last remaining observation window of gamma-ray astronomy from 10 TeV to several PeV. The main questions addressed by HiSCORE are cosmic ray composition and spectral measurements in the Galactic/extragalactic transition range, and the origin of cosmic rays via the search for gamma rays from Galactic PeV accelerators, the pevatrons. HiSCORE is based on non-imaging Cherenkov light-front sampling with sensitive large-area detector modules of the order of 0.5 m². A prototype station was deployed on the Tunka cosmic ray experiment site in Siberia, where an engineering array of up to 1km² is planned for deployment in 2012/2013. Here, we address the expected physics potential of HiSCORE, the status of the project, and further plans.

The Cherenkov Telescope Array (CTA) will be the next high-energy gamma-ray observatory. Selection of the sites, one in each hemisphere, is not obvious since several factors have to be taken into account. Among them, and probably the most crucial, are the atmospheric conditions. Indeed, CTA will use the atmosphere as a giant calorimeter, i.e. as part of the detector. The Southern Hemisphere presents mainly four candidate sites: one in Namibia, one in Chile and two in Argentina. Using atmospheric tools already validated in other air shower experiments, the purpose of this work is to complete studies aiming to choose the site with the best quality for the atmosphere. Three strong requirements are checked: the cloud cover and the frequency of clear skies, the wind speed and the backward trajectories of air masses travelling above the sites and directly linked to the aerosol concentrations. It was found, that the Namibian site is favoured, and one site in Argentina is clearly not suited. Atmospheric measurements at these sites will be performed in the coming months and will help with the selection of a CTA site.

In the presented work the results of GRBs temporal profiles analysis in the high energy gamma-band are discussed. Now GRBs high energy gamma-emission was observed both during short and long bursts mostly by detectors onboard Fermi and Agile satellites. The duration of such emission is more than some hundreds seconds and sufficiently longer than t₉₀ in the low energy band. But usually the maximum of high energy emission is in the t₉₀ intervals. However the investigation of GRBs temporal profiles in the region E>100 MeV have shown the opportunity of new burst type separation. In the difference of usual GRBs, temporal profiles of new type of bursts in the high energy gamma-band have several characteristic features. For example, GRB090323, GRB090328 and GRB090626 temporal profiles have additional maxima after low energy t₉₀ intervals finished. These bursts temporal profile analysis have shown that faint peaks in low energy bands close to the ends of low energy t₉₀ intervals preceded these additional maxima. The analogues features were separated during some other GRBs by the results of preliminary data analysis, for example, GRB110721A and GRB100724B. We suppose that these GRBs could be considered as different GRB type. The temporal profiles and spectra characteristic properties of new type of bursts are discussed in this article.

The results of the calculations of temperature coefficients for integral cosmic ray muon fluxes coming to the sea level (vertical and horizontal) with energies 10², 10⁴ and 3×10⁶ GeV are given. The calculations are made according to current data on production of pions, kaons and charmed particles obtained during studying proton-nucleus interaction at modern accelerators.

ANTARES is the largest Neutrino Telescope operating in the Northern Hemisphere. Placed at the bottom of the Mediterranean Sea, about 40 km off the coast of Toulon (France), it is composed by 885 photomultiplier-tubes (PMTs) which detect the Cherenkov light emitted in the interaction of high energy neutrinos close or inside the detector. One of the main goals of the experiment is the identification of a source of cosmic neutrinos, which are likely to be produced in the interaction of high energy hadrons in several astrophysical scenarios. The discovery of a source of neutrinos will be, thus, a clear indication for hadronic acceleration mechanisms and shed light on the problem of the origin of cosmic rays (CRs). This works present such a search using 813 days of data collected in ANTARES between years 2007 and 2010. Not having found any significance excess of events upper limits to the E_μ^−-2 are given for sources in the Southern sky. Additionally, results using specific emission models for two well known gamma-ray TeV sources are discussed.

Monte Carlo calculations were performed for two models of neutron detector. The first model of the neutron detector includes the layer of polyethylene as a moderator, boron as a target for (n, α) reaction and silicon as a detector of α-particles. The second model consists of polyethylene layers alternating with layers of plastic-boron scintillators. Calculations were performed for parallel neutron flux with evaporation spectrum. The calculation results of neutron detection efficiency for two proposed models were analyzed and compared. The high neutron detection efficiency is attained by using a plastic-boron scintillator. Using natural boron the 10% of detection efficiency is attained and in the case of enriched boron more than 15% of detection efficiency is attained when the detector thickness is 4 cm. The model using silicon detectors provides the detection efficiency about 4%.

Using the ANTARES neutrino telescope, the largest neutrino telescope in the Northern hemisphere, from its first configuration with 5 lines of photodetectors to the actual nominal one corresponding to a total of 12 lines, we have studied our ability to search indirectly an evidence of Dark Matter annihilations in heavy astrophysical objects as the Sun. First limits have been obtained using the data recorded by ANTARES in 2007 and 2008, and compared with neutrino fluxes predicted within a minimal supersymmetric extension of the Standard Model with supersymmetry-breaking scalar and gaugino masses constrained to be universal at the GUT scale, the CMSSM, as well as a minimal Universal Extra-Dimensions scenario with one extra compact dimension where all the Standard Model fields propagate into the bulk, the mUED. The current limits over the neutrino/muon fluxes coming from the dark matter self-annihilations, as well as the spin-dependent and spin-independent cross-sections, are presented.

A new installation HORIZON-T is commissioned at the high altitude scientific station of P.N. Lebedev Institute at the Tien-Shan Mountains. The purpose of this installation is to study EAS arriving at the zenith angles close to the horizon. The installation consists of three Vavilov – Cherenkov detectors located at the center of the installation and five registration points for muons which are placed within 500 m from the center. With the help of HORIZON-T installation EAS events have been detected at zenith angles more than 65 degrees, some of which had muon pulses with the front being ahead of one from Vavilov – Cherenkov pulses by more than 20 ns. Simulations show that such EAS are most likely initiated by primary nuclei with the mass more than 10.

Results of simulation of the spectra of cosmic rays (CR) on the Earth surface by means of the CORSIKA code are presented. For simulation, a standard model of the atmosphere and additional ones (with changed temperature profile and changed values of pressure at sea level) were used. Spectra of particles were obtained in the energy range 0.1 − 100 GeV for five values of zenith angle (0, 15, 30, 45 and 60 degrees) and, for the vertical direction, for several altitudes (0 m, 500 m, 1000 m and 1500 m above sea level). Barometric and temperature coefficients for various components of CR were estimated from the simulation data.

We show that nucleon electromagnetic structure functions of deep inelastic scattering in Regge-Gribov limit (fixed Q-squared, asymptotically large 1/x and s) can be well described in the two-component (soft + hard) approach. In the concrete model elaborated by authors, the soft part of the virtual photon-nucleon scattering is given by the vector meson dominance, with taking into account the radial excitations of the rho-meson and nondiagonal transitions in meson-nucleon interactions. The hard part is calculated by using the dipole factorization, i.e., the process is considered as the dissociation of the photon into a -pair (the "color dipole") and the subsequent interaction of this dipole with the nucleon. The dipole cross section has a Regge-type s-dependence and vanishes in the limit of large transverse sizes of the dipole. We give the brief description of the model and present results of the detailed comparison of model predictions with experimental data for electromagnetic structure functions of the nucleon.

Correction of the muon flux at the Earth surface for temperature effect with the help of two simple methods is considered. In the first method, it is assumed that major part of muons are generated at some effective generation level, which altitude depends on the temperature profile of the atmosphere. In the second method, dependence of muon flux on the mass-averaged atmosphere temperature is considered. The methods were tested with the data of muon hodoscope URAGAN (Moscow, Russia). Difference between data corrected with the help of differential in altitude temperature coefficients and simplified methods does not exceed 1-1.5%, so the latter ones may be used for introduction of a fast preliminary correction.

We present results from tests performed at Karlsruhe Institute of Technology (KIT) and at FermiLab Meson Test Beam Facility (FNAL) to study electron-muon separation, time of flight resolution and the acceptance for a new EAS detector concept. The very good time resolution and adjustable orientation of the detector permit to separate upward-moving tracks from downward tracks at any orientation with high efficiency. With these performances the detector can measure interaction products from cosmic neutrinos with zenith angles > 90 degrees, defining a chord through the earth as the interaction path. This kind of detector using SiPM will be a part of a large area array (several square kilometer) designed to measure UHE neutrinos (0.01-100 EeV).

The technique of single muon track reconstruction in Cherenkov water detector NEVOD is presented. The technique is based on the maximum likelihood method, in which probabilities of PMT response are used. The reconstruction technique has been tested on real experimental events selected by the coordinate detector DECOR. The angular distribution of detected muons has been estimated.

The ANTARES neutrino telescope is currently the largest water Cherenkov detector in operation in the Northern Hemisphere. The detector is a lattice of 885 Optical Modules distributed over 12 lines, located 40 km off the Southern French coast at a depth of about 2500 m. Its main scientific goal is the detection of high energy cosmic neutrinos from galactic and extra galactic sources using the Cherenkov photons emitted along the pattern of neutrino-induced charged leptons. The detector has been taking data regularly since 2006 in a partial configuration and has been completed in Spring 2008. The status of the experiment is reported and a selection of the latest results is discussed. In particular, this paper presents the up to date upper limits for diffuse high-energy cosmic neutrino flux, the searches for point sources, the multi-messenger analyses and the measurement of the neutrino oscillations.

The technique of cascade shower energy measurements by means of Cherenkov water detector (CWD) NEVOD with a spatial lattice of quasi-spherical modules (QSM) is discussed. A dense QSM spacing allows to reconstruct the number of cascade particles along the shower axis on the basis of amplitude responses of PMTs. The technique of cascade curve reconstruction was applied to showers generated in water by nearly horizontal high energy muons selected by means of the coordinate detector DECOR deployed around the CWD. First results of cascade energy spectrum measurements are presented.

A report is presented on the search for magnetic monopoles and nuclearites with the ANTARES experiment, using data collected in 2007 and 2008. A large light signal is expected from these presumably rare particles. The analysis of data yielded no exotic candidates, thus upper limits were set on the flux of fast upgoing magnetic monopoles and of slow downgoing nuclearites.

Precise measurements of the muon flux are important for different practical applications, in environmental studies and for the estimation of the water equivalent depths of underground sites. A first configuration of the mobile detector was composed of two 1 m² scintillator plates, each viewed by wave length shifters and read out by two PMTs (Photomultiplier Tubes). A more recent configuration of the mobile muon detectors, set up in IFIN-HH, Romania, consists of two 1 m² detection layers, each one including four 1×0.25 m² large scintillator plates. The light output in each plate is collected by twelve optical fibers and then read out by one PMT. The calibration has been made by comparing the energy deposit spectrum of minimum ionizing particles with the spectra simulated with the GEANT4 code. The device is used to measure the muon flux on different locations at the surface and underground.

A multidirecional high energy cosmic ray (muon) telescope is operational at the Southern Space Observatory, in Sao Martinho da Serra, RS, Brazil. This telescope is part of the Global Muon Detector Network (GMDN) and aims to study and forecast Space Weather. This paper proposes a new counting, correlation and recording solution based on an embedded system able to interface observational data by internet for remote monitoring. It is built around a Rabbit 3000 microcontroller with TCP/IP Ethernet 10Base-T connectivity. It is able to detect and count 200 ns pulses generated by the sensor system (scintillator plastics coupled with photomultipliers) during a specified period of time (generally one second). A preliminary version of a monitoring web page was developed and it is able to show the cosmic ray (muon) data of one detector in real time. The current system is an attempt to improve the reliability of the telescope when comparing to the recording system based on a personal computer, currently under operation. One advantage is the easy maintenance, since all the counting and correlation boards currently under operation can be replaced by an embedded system. Besides, as the hardware is off-the-shelf, it is only necessary to develop software routines, which is based on royalty-free libraries.

The negative atmospheric temperature effect observed in the muon intensity measured by surface-level detectors is related to the atmospheric expansion during summer periods. According the first explanation given, the path of muons from the higher atmospheric level (where they are generated) to the ground becomes longer, and more muons decay, leading to a muon intensity decrease. A significant negative correlation, therefore, is expected between the altitude of the equi-pressure surface and the muon intensity. We compared measurements of the altitude of 100 hPa equi-pressure surface and data from the multidirectional muon detector installed at the Brazilian Southern Space Observatory in São Martinho da Serra, RS. Significant correlation coefficient were found (up to 0.95) when using data observed in 2008. For comparison, data from the multidirectional muon detector of Nagoya, located in the opposite hemisphere, is studied and an anti-phase in the cosmic ray variation related with the temperature effect is expected between data from detectors of Nagoya and São Martinho da Serra. The temperature influence is higher for the directional channels of Nagoya than for ones of São Martinho da Serra.

The results of Monte-Carlo simulations of neutron production by muons in LVD obtained with Geant4 and SHIELD programs are presented. The detection efficiencies of gammas and neutons in the LVD are calculated.

LVD detector, located in Gran Sasso National Laboratory, has been working on the program of the search for neutrino radiation from gravitational collapses of stars since 1992. In 2005 additional modifications of the detector by adding NaCl target were made. For the last two years the experiment with one portatank (8 counters) of LVD has been under way. Monte-Carlo simulation and its comparison with experimental data are presented and discussed in this paper.

We present a current status of the Baikal-GVD Project. The objective of this project is a construction of a km3-scale neutrino telescope in the Baikal lake. Set of prototype arrays which were installed and operated during 2009-2011 in Lake Baikal allowed to study all basic elements of the future full detector and to finalize the GVD technical design. We discuss the configuration and the design of the engineering arrays as well as DAQ performance and the preliminary results.

Cosmic ray muons stopped in 5 cm thick plastic scintillators at surface and at depth of 25 m.w.e are studied. Apart from the stopped muon rate we measured the spectrum of muon decay electrons and the degree of polarization of stopped muons. Preliminary results for the Michel parameter yield values lower than the currently accepted one, while the asymmetry between the numbers of decay positrons registered in the upper and lower hemispheres appear higher than expected on the basis of numerous earlier studies.

Using the method of spectrographic global survey, rigidity spectrum and anisotropy of galactic cosmic rays during GLE on 14 July 2000 have been studied with the data from ground-based observations of cosmic rays (CR) at the world-wide network of stations. The CR rigidity spectrum observed during this period over the range 1 to ~ 20 GV is shown to be described not only by power function of particle rigidity: distribution of CRs in the earthward direction varies with time and depends on their energy.

We studied variations in the galactic cosmic ray (CR) rigidity spectrum and anisotropy during the July 2000 strong magnetic storm from the ground-based observations of cosmic rays within the world network of neutron monitor stations through spectrographic global survey. We show the time history for amplitude variations in the rigidity spectrum of cosmic rays, their anisotropy and planetary system of the geomagnetic cutoff rigidity during the Forbush-effect evolution over that period.

The paper presents findings of rigidity spectrum of cosmic ray (CR) variations during certain Forbush decreases recorded at the worldwide network of neutron monitors over the period 1991-2005. In the majority of events under consideration, rigidity spectrum of primary CR variations is not described by the power function of rigidity over the energy range to which neutron monitors are most sensitive.

The meteorite data on monitoring of the GCR gradient variations at 2-4 AU from the Sun in 1957-2010 testify to the influence of the character of the solar magnetic field inversions during the maximum of the solar cycles on depth of the GCR modulation in the heliosphere.

Key explanation on effect of Fundamental Law of Momentum Conservation is given on the basis of Cosmo-Physical processes, which can be connected with all kinds of recently known geo-effective phenomena. Many works have been devoted to searches of extraterrestrial sources of generation of earthquake initiation preconditions. There is a direct indication on the fact in these works that all kinds of geo-active fluxes of plasma, which goes ahead of strong geomagnetic storms, concomitant to the earthquakes, may be served as favourable conditions for earthquake appearance. If in one group of works, the increase of seismic activity during geo-active solar flare is reported, then in the other group of works, there is the direct indication on the fact, that it is necessary to study the mechanism of generation of electro-magnetic emanation in the seismically active regions of Earth. Certain strong destructive earthquakes are putting in touch by some authors with the outburst of cosmic rays in distant regions of Universe during stellar explosion of supernovae. It's impossible to avoid our attention from announcement of 100% increase of hard component of cosmic radiation above Yerevan 30 minutes ahead of 1988 Spitak Earthquake. And finally, the data on article, in which is shown that about 75% of earthquakes with magnitude M≥6 takes place during traverse of neutral layer of Interplanetary Magnetic Field by the Earth, in the presence of good correlation with 11-years cycle of Solar Activity. Above mentioned geo-effective phenomena, with an increasable amount, can be reviewed in frame of the Law of Momentum Conservation, if we take into account the peculiarities of its development for a given specific cases.

Studying the solar proton events of 2012 on January 27 and May 17 we apply methods elaborated previously. The results are compared with those obtained for the events of 2006 December 13 and 14. The onset of microwave emission at 15.4 GHz has been chosen as a zero time moment for each parent solar flare. Emission measure of flare plasma started its exponential increase at zero time. The onsets of 100 MeV solar protons in these four events have been registered by the GOES detector after 30-35 min after to the zero time. Temporal profiles of ~100 MeV proton intensities can be fitted by the diffusion propagation model with mean free path of ~0.1 a.u. and prolonged source functions with several episodes of different injection rate into the heliosphere. These methods are not applicable for poor connected SEP events as the event on March 7, 2012.

The numerical model of the shock-drift acceleration of interstellar pick-up protons at the solar wind termination shock is presented taking into account multiple reflections of the particles at and passing through the shock. The processes of the multiple interactions with the shock are possible due to pitch-angle scattering in the upstream and downstream parts of the solar wind flow. The model takes into account variations of the magnetic field direction near the shock front connected with its three-dimensional shape. The main advantage of the model is the self-consistent treatment of protons and interstellar hydrogen atoms, which interact with each other through the resonant charge exchange process. The model gives very simple and natural resolution of so-called injection problem for anomalous cosmic rays. The shock-drift acceleration can explain the fluxes of the anomalous cosmic rays measured at the Voyager 1/2 spacecraft after the termination shock crossings.

We analyze relations between characteristics of an extended ensemble of Forbush decreases (FDs) caused by CMEs from the central zone of the solar disk during the 23rd solar cycle, on the one hand, and such solar eruption parameter as a summarized unsigned magnetic flux of CME-associated EUV dimmings and arcades, on the other hand. This eruption parameter is shown to have a pronounced direct correlation with the FD magnitude and a conspicuous reverse correlation with the ICME transit time from the Sun to the Earth. The revealed correlations indicate that main quantitative characteristics of major non-recurrent FDs (and geomagnetic storms as well) are largely determined by parameters of solar eruptions, in particular such as the summarized magnetic flux of dimmings and arcades.

Appearance in the solar atmosphere of high-energy protons during major solar flares can be identified from the observation of a broad gamma-ray line in the 70-100 MeV range of the flare emission spectrum. This emission line results from the decay of neutral pions, which, in turn, are produced in interactions of high-energy (> 300 MeV) protons with dense layers of the solar atmosphere. We considered 12 events with clear observations of the pion-decay gamma emission and compared the light curves of this emission with time profiles of different emissions. In 9 events out of 12 we found the onset and peak times of high-energy gamma-rays to be close to the peak times of other electromagnetic emissions and the derivative of the soft X-ray emission. This closeness indicates that efficient acceleration of protons up to sub-relativistic energies starts typically close to the time of the main flare energy release. The further study dealt with the data recorded since 1972 by the world neutron monitor network related to 44 Ground level enhancements (GLEs) and light curves of neutral emissions of the associated flares. The study revealed that a delay of the earliest arrival time of high-energy protons at 1 AU with respect to the observed peak time of the solar bursts did not exceed 10 min in 30 events. This result indicates that in the majority of events, efficient acceleration of protons responsible for the GLE onset should be close to the time of the main energy release in flares.

Computation of solar energetic particles propagation in the magnetosphere and atmosphere of the Earth is very important for ground level enhancement analysis. Detailed simulations of solar energetic particles events starting from asymptotic direction computation and NM detector response make it possible to build a strategy for inverse problem solution i.e. obtaining the characteristics of solar energetic particles on the basis on ground measurements. In this study a simulation of cosmic ray atmospheric cascade is carried out with PLANETOCOSMICS code. Energy spectra of secondary particles, namely neutrons and protons are obtained at various altitudes in the rigidity range of 0.7 GV to 1 TV of primary particles. Considering updated results for NM-64 detection efficiency the specific yield function for the standard neutron monitor is obtained for vertically and obliquely incident primary particles. The obtained results and applications are discussed.

Modernisation of the hardware-software complexes of CR stations worldwide in order to work in the real-time mode is a topical problem. Solution to this problem will promote diagnostics of solar-terrestrial relations and space weather forecast. Complex and online analysis of data on CR variations requires full automation of primary data processing, timely data entry into databases with online update, and free access to data. The paper presents characteristics of CR stations of ISTP SB RAS. We describe the hardware-software registration complex which was updated in order to do work in the real time mode. Detailed consideration is given to transmission systems of data from CR stations of ISTP SB RAS and to antenna systems. We give examples of creating databases on the server of CR station Irkutsk and remote CR stations of ISTP SB RAS, and their synchronisation. We also present the existing international projects, which deal with database development, and the participation of CR stations of ISTP SB RAS in these projects (Irkutsk, Irkutsk 2, Irkutsk 3, Norilsk).

Standard model of galactic cosmic rays (GCR) propagation in heliosphere and adjacent interstellar space is considered. Here heliosphere is considered as a two-layered medium consisting of two spherical regions symmetrical about the Sun and adjacent to each other. In the internal region of the heliosphere, which is bounded by termination shock, solar wind has supersonic speed, and in the external region, which is bounded by heliopause, solar wind has subsonic speed. GCR scattering in these regions is happening in different ways and is characterized by corresponding diffusion rates. In the interstellar medium speed of the solar wind is supposed to be equal to zero and scattering became more weak. Here we suppose that there are no any sources of particles on the boundaries between layers. Exact analytical solution of corresponding mathematical problem is not difficult in principle, but is exceedingly bulky, therefore in this work analytic expressions are obtained both for high energy particles (>2500 MeV) and for low energy particles (<1400 MeV) for each region of their propagation. Distribution of the low energy particles confirm to results obtained on the «Voyager» spacecrafts. It is shown that irrespective of the scattering conditions in internal and external parts of the heliosphere density of the low energy particles is continuously growing from the Sun to the heliosphere boundaries.

The time profiles of the galactic cosmic ray intensity near the Earth are considered. We try to reproduce the main features of these profiles by solving the usual boundary–value problem with the transport equation and rather simple models of its coefficients. Only the "normal" 22-year cycle consisting of the pair of the successive 11-year cycles in the GCR intensity (1980-2000) is discussed. Besides, we suggest the method to decompose the intensity into the partial "intensities" connected with the main physical processes.

We compare the different approaches (observational and theoretical) to the definition and separation of the GCR intensity variations due to the changing number and area of sunspots (the sunspot cycle) and the changing polarity of the high-latitude solar magnetic fields (the magnetic cycle). Using the theoretical approach we can consider how both types of the GCR intensity variations change with energy in different parts of the heliosphere during the minima of the sunspot cycle and their relative weights in the calculated intensity.

Using Monte Carlo method we have simulated solar cosmic ray spectra (³He, ⁴He, O and Fe) at the flare site and at the Earth. It is shown that besides stochastic acceleration by Alfvenic turbulence an impulsive electric field of the current sheet significantly affects the ion energy spectra at low energies. Both mechanisms could explain some peculiarities in the energy spectra of heavy ions observed in experiments onboard ACE.

Aims. We analyze the kinematics of three interplanetary coronal mass ejections (ICMEs) that occurred on 13th, 14th and 15th February 2011 in the active region AR 11155 and have shown that they appeared at the Earth orbit on February, 18th and caused Forbush decrease (FD). Methods. The solar coordinates of flares are (S19W03), (S20W14) and (S21W18). The kinematic curves were obtained using STEREO (A&B) data. Additionally, we explore the possibility of the CME-CME interaction for these three events. We compare obtained estimates of ICME arrival with the in-situ measurements from WIND satellite at L1 point and with ground-based cosmic ray data obtained from SEVAN network. Results. The acceleration of each CME is highly correlated with the associated SXR flares energy release. CMEs that erupted at 13 and 14 Feb 2011 are not associated with prominence eruption; maximum velocity was v_max550 ± 50 km/s and v_max400 ± 50 km/s, respectively. However, 15 Feb 2011 CME is connected with much more violent eruption associated with a prominence, with maximum velocity of v_max 1400 ± 50 km/s. The last overtakes 13th and 14th Feb CMEs at distances of 32 and 160 R⊙, respectively.

High energy particles of galactic and solar origin crossing a spacecraft affect experiment performance in space. At time scales of tens of minutes, galactic cosmic-ray (GCR) energy fluxes vary of a few percent at most. Conversely, solar energetic particle (SEP) fluxes may vary of several orders of magnitude during the same periods of time. In order to study accurately the effects of the incident solar particles on future space experiments, a good knowledge of particle energy distribution during the whole duration of SEP events is necessary. We report here the parameterization of proton and helium energy spectra observed during SEP events of different intensity at energies above 100 MeV/n. We benefit of both data inferred at the top of the atmosphere from ground neutron monitor observations and recent measurements gathered by the PAMELA cosmic-ray experiment carrying a magnetic spectrometer in space.

The prolonged 23 cycle minimum has been tested on the basis of introduced by us the fluctuation parameter of galactic cosmic ray (GCR) intensity. Long-term forecast of the onset of new (24) 11-year cycle with an advance of ~1 year is given. Besides, a middle-term forecast of activity growth phase of the new 24 cycle with the advance of ~1 Sun rotation is presented. From results of the wavelet-analysis it follows that a low-frequency drift of 11-year cycle period has begun as long ago as the 22 cycle. It is necessary to notice that we have predicted the failure of 11-year cycle period (by our terminology it is called a «low-frequency drift» [3]) 3 years prior to its obvious manifestation in 2008-2010. Results of a trajectory analysis of GCR fluctuation parameter on a complex phase plane indicate that the greatest area is "covered" with a trajectory of the same 22 cycle. It is believed (in the view of G.V. Kuklin, 1982) that the greatest area of phase trajectory is an evidence of abnormal cycle before a «phase catastrophe». It is obvious that since the 22 cycle the prolonged failure of 11-year cycling has begun.

It is established, that the main contribution into dynamics of galactic cosmic ray intensity fluctuations (GCR) in a vicinity of magnetic "cork" from a shock gives a nonrandom, non-Gauss component of GCR intensity. An occurrence of correlated fluctuations is caused by following circumstance: due to laws of conservation the probability that the cosmic ray particles reflected from a magnetic cork (in the expanding magnetic field) will undergo collimations, becomes considerable. The collimation will be manifested in focusing of particles into the anisotropic beams. In this case, observations should show "scintillations" of celestial sphere in cosmic rays i.e. the" HALO" effect. Similar scintillations are the indicator of interplanetary magnetic cork. The algorithm of detection of GCR scintillations is realized in real time using "Cyber-FORSHOCK" robotized system.

The presence of Jovian electrons at the Earth orbit allows considering them as test particles probing of the structure of the inner heliosphere. The penetration of Jovian electrons into the inner heliosphere during periods of optimal magnetic connection between Jupiter and Earth is trivial phenomenon, while a special magnetic configuration is necessary for periods when such a connection is absent. The possibility of the formation of long-living CIR-like magnetic traps filled by low-energy electrons (~ 1 MeV) during their passage by Jupiter and their subsequent arrival at the Earth is considered.

According to the SOHO > 0.25 MeV Jovian electron data during solar activity minimum in 2007–2008 the structure of the solar wind and its steady-state allowed the formation of such traps, existing for about a year (14 solar rotations).

There are some special directions in the interplanetary space, which are set by the solar wind velocity and position of the interplanetary magnetic field lines. Due to this a strongly inhomogeneous distribution of the phases and amplitude-phase interrelation appear in the first harmonic of the cosmic ray anisotropy. To study the long term variations of cosmic ray anisotropy the characteristics of its first harmonic defined for each hour by global survey method have been used throughout the period 1957-2010. For each year of this period longitudinal distribution of the cosmic ray vector anisotropy and its amplitude-phase relation were obtained. The results clearly demonstrate the dependence of cosmic ray anisotropy variations on the solar activity and solar magnetic cycles. Periods of specific behavior of the anisotropy are extracted and discussed. The results by this study obtained are consistent with the convection-diffusion model of the anisotropy.

In the present paper the comparison of the results of the simultaneous measurements of solar proton fluxes on board geostationary satellites "GOES" and "Electro" was made for the purpose of calibration of "Electro-L" detectors and determination of the possibility to utilize "Electro-L" data for space weather monitoring. It was shown that the solar proton observation data on board "Electro-L" recalculated to energy thresholds of "GOES" 10 and 30 MeV are in a good consistent with "GOES" data and may be used for control of radiation conditions in near-earth space.

The abnormally high solar activity was observed in the late 50's – the early 60's of the 20th century, but not many possibilities was available that time of its observation to which we have got in use during the last years. Ground level cosmic ray observations, along with geomagnetic activity, are one of a few kinds of the continuous measurements, allowing to judge on the events of 19th cycle. The IZMIRAN Database in which all Forbush-decreases are collected since July, 1957 has been used for the analysis. To make the statistics of 19th cycle fuller, the catalogue by Lockwood containing rather big Forbush-decreases (>3 %), picked out from the data of one neutron monitor (Mount Washington), was involved. Comparison of the events in cosmic rays with solar and geomagnetic activity has shown that the quantity and intensity of geomagnetic storms in 19th cycle correspond to abnormally high number of the sunspots. However in this cycle there is a certain deficiency of Forbush-effects of the large size. Apparently, deficiency of the big Forbush-decreases during this period means that coronal mass ejections (CMEs/ICMEs) in the 19th cycle distinguished from later CMEs and differently affected of the cosmic ray modulation and geomagnetic activity. Probably, the most powerful CMEs of the 19th cycle had, as a whole, the smaller size, than the greatest emissions of solar plasma in later period.

The radiation dose rates at flight altitudes can increase by orders of magnitude for a short time during energetic solar cosmic ray events, so called ground level enhancements (GLEs). Especially at high latitudes and flight altitudes, solar energetic particles superposed on galactic cosmic rays may cause radiation that exceeds the maximum allowed dosage limit for the general public. Therefore the determination of the radiation dose rate during GLEs should be as reliable as possible. Radiation dose rates along flight paths are typically determined by computer models that are based on cosmic ray flux and anisotropy parameters derived from neutron monitor and/or satellite measurements. The characteristics of the GLE on 15 April 2001 (GLE60) were determined and published by various authors. In this work we compare these results and investigate the consequences on the computed radiation dose rates along selected flight paths. In addition, we compare the computed radiation dose rates with measurements that were made during GLE60 on board two transatlantic flights.

The main characteristics and course of the current solar cycle XXIV evolution after 3.8 years of development and some signs suggesting that the current cycle is in a phase of maximum are considered. At the same time, the curve of the current solar cycle evolution is similar to the solar cycle XIV – the lowest of the authentic solar cycles. During the current solar cycle 30 large solar flares have occurred up to now, among which two flares with the class X> 5 and 13 flares with class X≥1.0. The number of geoeffective solar flare events and coronal holes is abnormally low. During the period no several magnetic storms (Ap ≥ 100), only one major magnetic storm (Ap ≥ 70), two solar proton event (E_pr> 10 MeV) with a flux of protons greater than 1000 p.f.u. and only one GLE event were registered.

The origin of 0.03-1 MeV/nucleon ions is investigated on the basis of ULEIS (ACE) data during quiet time periods in 1998-2011. The energy spectra of ³He, ⁴He, O, and Fe ions and the energy dependence of their relative abundances are obtained. The comparison of Fe/O abundance ratios during quiet time periods with the average relative ion abundances in various phenomena of solar activity shows that the ion fluxes tend to split into 3 groups. Over the entire solar cycle excluding minimum the Fe/O values corresponded to those observed in impulsive solar energetic particle (SEP) events (group I) and in the solar corona (group II). Near the activity minimum, however, the Fe/O values were usually near their solar wind values (group III). The energy spectra of suprathermal ions and the energy dependence of ion abundance ratios in different groups are also different depending on the ion first ionization potential. These results suggest that various acceleration mechanisms are at work in the different groups. The nearly constant values Fe/O 1 and ³He/⁴He 0.065 up to 0.8 MeV/nucleon obtained for ion group I possibly result from ion acceleration in small impulsive SEP events rich in Fe and ³He. This ratio Fe/O is about 15 times higher than the photospheric value and corresponds to the Fe abundance in the upper corona in old active regions. We suggest that ions in these coronal regions represent the population accelerated in impulsive SEP events.

The method for determination of the long-term rigidity spectrum of the cosmic ray (CR) variations within the range R=1-50 GV was presented in our previous works on the base of CR observations with the different detectors. In this paper meson telescope data (Nagoya) are added. The monthly averages of the CR intensity during 1974-2011 are used to investigate rigidity spectrum of the CR maximum in 24th cycle and compare with other cycles. The main focus is specific features of CR modulation at a prolonged minimum of solar cycle 24, when maximum CR intensity was higher than it was during the other maxima. It has been found the best fitting for rigidity dependence of CR variations. The main results are: a) the power of the 11-yr cycle is different from one cycle to next; b) the maximum 24th cycle (2009) exceeds the previously established maximum flux of CR; c) the spectral index, obtained from different sets of CR detectors, shows that resulting spectrum becomes steeper with increasing of CR energy

The galactic cosmic rays (CR) are the main ionization source at altitude of ~ 3 to 35 km in the atmosphere. An analytical model is proposed, which describes the intensity of galactic cosmic rays in the inner heliosphere (where energy losses have important role) and the outer heliosphere (where convection-diffusion processes are dominant) [Buchvarova et al, 2011]. On the base of computed model parameters for 1 AU integral CR spectra D(>E) for the Earth and outer planet are obtained at solar minimum and maximum. The obtained results are compared with experimental data and theoretical results.

In order to obtain rigidity spectra from the ~40 stationary neutron monitors around the world, two calibration neutron monitors were built in 2002. Various tests were performed on these neutron monitors, and some calibrations have been done. Due to electronic development during the past ten years, the electronics heads were completely redesigned and rebuilt in 2011. The progress and results of the calibration effort, as well as plans for a network of mini neutron monitors, are reported.

In our previous works we have created the method of determination of parameters of cosmic ray daily anisotropy in the interplanetary environment based on the data provided by only single station – cosmic ray spectrograph named after A.I.Kuzmin. This method allows to predict the ingress of the Earth into large-scale solar wind disturbances with a probability of more than 70% and in advance time of about from several hours up to 2 days. Now it became possible to use the data of the neutron monitor networks, which can be seen in the neutron monitor database (NMDB) in real time. In this case the well-known method of global survey is applied for determination of cosmic ray anisotropy. Usage of the data of the cosmic ray station network allows to determine parameters of daily cosmic ray anisotropy with a greater accuracy.

By data of the neutron monitor worldwide station network the events of ground level enhancements of solar cosmic rays are studied. The absolute flow J and the energy spectral index γ of solar cosmic rays during the isotropic phase for 14 GLE events observed for 1977-2006 have been estimated using the method of effective energy by [1]. It is shown that in these events the changes of the power spectral index in the range from 3 to 7 are observed. It is noted that for the individual events the index about 5 is observed for a long time.

On the basis of long-term registration of cosmic rays with the muon spectrograph at Yakutsk (62°01'N, 129°43'E) and multidirectional muon telescope at Nagoya (35°10'N, 136°58'E) the cosmic ray semidiurnal variation seasonal change and the change of cosmic ray semiduirnal variation with the solar activity level has been found. The modeling of the seasonal change has been made.

Based on data of long-term measurements of muon intensity at the surface and underground on the depth of 7, 20 and 60 m w.e. at Yakutsk (62°01'N, 129°43'E) the sidereal and antisidereal variations of galactic cosmic rays during periods of positive and negative epochs of the general magnetic field of the Sun.

We compare the current characteristics of the sunspot activity and cosmic ray intensity with those expected in the future maximum of the current solar cycle. The values for maximum phase are estimated from the correlation between characteristics in the maximum and in the inflection points (few years before maximum) for the previous solar cycles. The expected galactic cosmic ray phenomena typical for the maximum phase of solar cycle (Gnevyshev Gap effect, quasi-biannual oscillations and energetic hysteresis) are discussed.

We have suggested a model of magnetic cloud presented as a torus with magnetic flux rope structure situated inside the interplanetary corona mass ejecta expanding radially away from the Sun through the interplanetary medium. The magnetic field of the torus changing during its propagation has been obtained. The magnetic cloud — solar wind boundary transparency for cosmic rays with different energies depending on the cloud orientation and properties of the torus magnetic field has been determined by means of calculation of the particle trajectories at the boundary.

We have developed the calculation method of the cosmic ray intensity anisotropy dynamics near the solar wind disturbance. Possible variants of the dynamics for different conditions have been presented.

One of the most important data corrections related to the primary data processing of the neutron monitors is the pressure correction due to the barometric effect. This effect induces considerable variation in the counting rate of a cosmic ray detector which is not related to the real variation of the cosmic rays flux but only to the local atmospheric pressure of the station. In order to provide the worldwide neutron monitor network with good quality data, a correction has to be made that requires the calculation of the barometric coefficient. A new method that effectively calculates the barometric coefficient for a station using data of a reference station in order to subtract the primary variations of cosmic rays is presented in this work. Moreover, this method is the prototype of an online tool that uses data of the NMDB stations and calculates the barometric coefficient for any available station. This tool is also presented.

Here we present a method to forecast the arrival of an interplanetary shock to the Earth's orbit in advance of up to one day, using cosmic ray fluctuations and solar wind parameters measured onboard the ACE spacecraft. The method is based on our previous results [1]. By means of continuous monitoring of the interplanetary space state since April 2010, we conclude that not all shocks can be reliably forecasted by the method. Only those interplanetary shocks, for which a large flux of low-energy particles (10 keV − 10 MeV) of solar or interplanetary origin exists in the upstream region, can be forecasted. This is typically related to quasi-parallel shocks. In the absence of such particles, a forecast cannot be made. This is a typical situation for quasi-perpendicular shocks. Our analysis shows that, on average, an interplanetary shock can be forecasted for several hours up to one day, with the probability about 70%.

The effect of high-speed solar wind streams from low-latitude coronal holes on cosmic ray intensity is studied. The database on Forbush effects created at IZMIRAN, with cosmic ray density and anisotropy calculated by the Global Survey Method (GSM) on the basis of Neutron Monitor network data has been used for the entire 2007. From the analysis of events in 2007 it was found that relationship of the Forbush effect magnitude to the solar wind speed is much weaker than to the magnitude of the interplanetary magnetic field. Best of all the FE magnitude correlates with a 'critical' rigidity of the CR determined by the magnetic shield created by interaction of the high speed streams from coronal holes with low speed solar wind.

It is suggested in many studies that the pre-increases or pre-decreases of the cosmic ray intensity (known as precursors) which usually precede a Forbush decrease could serve as a useful tool for studying space weather effects. The events under consideration in this particular investigation were chosen based on two criteria. Firstly, the heliolongitude of the solar flare associated with each cosmic ray intensity decrease was in the 50°–70°W sector and secondly, the values of geomagnetic activity index (Kp_max) were ≥ 5. As a result only Forbush decreases connected to western solar flares and accompanied by a geomagnetic storm were selected. In total 25 events were gathered for the time period from 1967 to 2006. For the detailed analysis of the aforementioned cosmic ray intensity decreases data on solar flares, solar wind speed, geomagnetic indices (Kp and Dst) and interplanetary magnetic field were used. The asymptotic longitudinal cosmic ray distribution diagrams for all events were plotted using the "Ring of Stations" method. The results revealed clear signs of precursors in 60% of selected events.

The calculations of the heliolongitudinal dependence of solar proton peak intensities for protons with energy more than 30 MeV were made. The new method of analysis of a posteriory probability of SPE observations with the proton peak intensities more than the given intensity by condition of observation the associated solar X-ray bursts with peak intensities more than the given intensity was used. It was shown that the heliolongitudinal peak intensity decrease for the event with flares in the western half of solar disk is practically absent, for heliolongitudinal interval from 0⁰ up to 30⁰ E is equal to 30 and for heliolongitudinal interval 30^0–90⁰ E is equal to100-150.

Forbush decreases (Fd) of the galactic cosmic ray (GCR) intensity and geomagnetic storms are observed almost at the same time. Geomagnetic storm is a reason of significant disturbances of the magnetic cut off rigidity causing the distortion of the time profile of the Fd of the GCR intensity. We show some differences in the temporal changes of the rigidity spectra of Fd calculated by neutron monitors experimental data corrected and uncorrected for the changes of the geomagnetic cut off rigidity. Nevertheless, the general features of the temporal changes of the rigidity spectrum of Fd maintain as it was found in our previous investigations. Namely, at the beginning phase of Fd rigidity spectrum is relatively soft and gradually becomes hard up to reaching the minimum level of the GCR intensity; then the rigidity spectrum gradually becomes soft during the recovery phase of Fd. We also confirm that for the established temporal profiles of the rigidity spectrum of Fd a structural changes of the interplanetary magnetic field turbulence in the range of frequencies, 10^−-6÷10^−-5 Hz are responsible.

The CARPET cosmic ray detector was installed on April 2006 at CASLEO (Complejo Astronmico El Leoncito) at the Argentinean Andes (31.8S, 69.3W, 2550 m, Rc=9.65 GV). This instrument was developed within an international cooperation between the Lebedev Physical Institute RAS (LPI; Russia), the Centro de Radio Astronomia e Astrofsica Mackenzie (CRAAM; Brazil) and the Complejo Astronmico el Leoncito (CASLEO; Argentina). In this paper we present results of analysis of cosmic ray variations recorded by the CARPET during increased solar flare activity in 2011-2012. Available solar and interplanetary medium observational data obtained onboard GOES, FERMI, ISS, as well as cosmic ray measurements by ground-based neutron monitor network were also used in the present analysis.

We present and discuss the ionosphere behavior under the impact of two X-ray solar flares (M8.7 and X1.7) that occurred on January 23 and 27, respectively, and were accompanied by Solar Proton Events (SPEs). The ionosphere response to these solar phenomena was detected using riometers (30 and 38.2 MHz), ionosonde and VLF systems operating at the Comandante Ferraz Brazilian Station in Antarctica and at the Itapetinga Radio Observatory in São Paulo (SP)/Brazil. The results suggest the ionosphere was affected by both SPEs, as evidenced by absorption detected in the cosmic noise, F2 layer critical frequency and VLF amplitude measurements. These absorptions started before the beginning of the main X-ray flare events and > 100 MeV proton events detected by GOES, suggesting the ionosphere was impacted by protons with energies above 2 GeV in Antarctica and above 10-12 GeV in SP as estimated from the particle geomagnetic rigidity (Rc) at each place. The results also suggest a long-lasting presence (hours) of high energy protons.

The cosmic ray component in the range of energies below 15 GeV is strongly affected by transient phenomena related to solar activity. Cosmic rays and solar particles with energies between 0.5 and 15 GeV can be observed by neutron monitors at ground level. In absence of solar activity, the background counting rate registered by neutron monitors is dominated by the galactic cosmic ray component, showing only long-term variations correlated with the solar cycle. During active periods, short-term temporal variations can be observed in close association with solar activity phenomena such as flares and coronal mass ejections. Most of these transients can produce a strong response in the magnetosphere. The aim of this work is to study the relationship between neutron monitor measurements and the magnetospheric response observed in Dst index, paying special attention to their connection with solar transient phenomena during the current rising solar activity phase.

The PAMELA magnetic spectrometer launched in June 2006 has observed the last strong energetic solar particle event of the 23rd solar cycle in December 2006. Subsequent long minimum of solar activity and weak development of the 24th solar cycle led to a deficit in the solar energetic particle events on the Earth orbit. As a result, only few events with protons accelerated above 100 MeV occurred in 2010-2012. The paper gives the preliminary results on energetic solar particles in the beginning of the 24th solar circle as measured with the PAMELA instrument.

Results of the study of variations of cosmic ray muon flux at the Earth surface during Forbush decreases (FD) registered in 2006 – 2011 by means of muon hodoscope URAGAN both for the integral counting rate and for different angular intervals are presented. Dependences of the amplitude of the decrease of cosmic ray muon intensity on the energy of primary particles in the energy region above 10 GeV during different phases of the FD were obtained. On the basis of the analysis of spatial-angular distribution of muon flux, values of the horizontal projections of the local anisotropy vector were calculated and their dynamics was studied. Energy, angular and temporal characteristics of Forbush decreases determined from cosmic ray muon data are compared with basic parameters characterizing conditions of near-Earth space before and during FD.

Forbush decrease was recorded for the first time with a global net of the neutron scintillation detectors (en-detectors) developed in INR RAS. The detectors are located at four geographic points: Baksan (43E, 43N), Gran Sasso, Italy (13E, 42N), Moscow (37E, 56N) and Obninsk (38E, 55N). This experimental fact by itself shows not only the possibility of using the detectors for cosmic ray variations study but also unbiasly supports the nuclear physics method developed by us as a novel instrument both for geophysical researches and for neutron environment monitoring.

We consider the cosmic ray modulation parameter exp(-V/λ) including V as the solar wind velocity and λ as the cosmic ray diffusion path in the interplanetary space. On the other hand, in the minimum of solar activity, the tilt angle of heliospheric current sheet α was used as possible characteristic of drift influence on cosmic ray intensity. We found that in the time periods around minima of solar activity the two parameters are in a rather strong anticorrelation, both facilitating the cosmic ray access into the inner heliosphere in the periods with the negative magnetic field in the northern hemisphere of the Sun.

Muon diagnostics is a technique of remote monitoring of various dynamic processes in the heliosphere, the magnetosphere and the atmosphere of the Earth based on the analysis of spatial-angular and temporal variations of muon flux simultaneously detected from all directions of the upper hemisphere. The developed approaches to data analysis and results of the study of various terrestrial and extra-terrestrial processes detected by means of a wide aperture URAGAN muon hodoscope are discussed.

Intensity of the atmospheric muon flux depends on a number of factors: energy spectrum of primary cosmic rays (PCR), heliospheric conditions, state of the magnetosphere and atmosphere of the Earth. The wide-aperture muon hodoscope URAGAN (Moscow, Russia, 55.7° N, 37.7° E, 173 m a.s.l.) makes it possible to investigate not only variations of the intensity of muon flux, but also temporal changes of its angular distribution. For the analysis of angular distribution variations, the vector of local anisotropy is used. The vector of local anisotropy is the sum of individual vectors (directions of the reconstructed muon tracks) normalized to the total number of reconstructed tracks. The vector of local anisotropy and its projections show different sensitivities to parameters of the processes of modulation of PCR in the heliosphere and the Earth's magnetosphere, and the passage of secondary cosmic rays through the terrestrial atmosphere. In the work, results of the analysis of long-term variations of hourly average projections of the vector of local anisotropy obtained from the URAGAN data during experimental series of 2007-2011 are presented.

Spectrometers PAMELA and ARINA, mounted on the spacecraft Resurs-DK1, carried out precision measurements of galactic cosmic ray (GCR) flux near the Earth from 2006 to present. Combining these instruments gives the possibility to study the effect of solar modulation in the energy range from 30 MeV to dozens of GeV. This report presents experimental results concerning the time interval from the end of the 23rd solar cycle (noted by an prolonged minimum) to the beginning of the 24th cycle. The cosmic ray flux raised up to the end of 2009, then it began to decline, which is in coincidence with the sunspot number and evidence of the solar activity increasing. Some additional features were noted in the time profile of galactic cosmic ray flux, which, as shown by analysis of the correlation, correspond to a change of such heliospheric parameters as the tilt angle of the heliospheric current sheet (HCS), the solar wind velocity and the intensity of interplanetary magnetic field (IMF).

Experimental data on cosmic ray fluxes measured in the stratosphere of polar and middle latitudes and their consistency with the heliospheric magnetic field strength and the solar wind velocity are discussed. During the last solar minimum the highest cosmic ray fluxes in the atmosphere were observed in 2009-2010. After prolonged solar minimum between the cycles of 23 and 24 the heliospheric magnetic field and the solar wind velocity recovered more slowly as compared with the values in the previous solar minima and remained substantially reduced in 2009-2012. As a result the cosmic ray fluxes are at present significantly higher than fluxes in the similar phases of previous solar activity cycles. The possible reasons of the existence of the long-term high fluxes of cosmic rays are discussed.

The features of the study of heliospheric disturbances on the basis of ground level cosmic ray muon flux observations are discussed. The muon hodoscope URAGAN simultaneously detects muons from various directions of the celestial hemisphere. This allows us to analyze spatial-angular variations of muon flux during such events. Heliospheric disturbances that caused the changes of interplanetary magnetic field parameters measured by various space vehicles are considered. A special attention is paid to the analysis of the response of the muon hodoscope URAGAN for recent most powerful solar flares that occurred in March 2012. In accordance with the results of the study, methods of separating main heliospheric disturbances are proposed. The prognostic potential of the developed approaches to the study of heliospheric disturbances by means of the penetrating component of cosmic rays is evaluated.

Geomagnetic conditions in near-Earth space have been a constantly evolving scientific field, especially during the latest years when the dependence of our everyday life on space environment has significantly increased. The scientific community managed to implement centers for the continuous monitoring of the geomagnetic conditions which resulted into short and long term forecasting of the planetary geomagnetic index Ap. In this work, the centers that have been established and are in operational mode in Russia (IZMIRAN), Greece (Athens), Kazakhstan (Almaty) and Bulgaria (Sofia) are presented. The methods that have been used for the forecasting of Ap index are demonstrated and the forecasted results in comparison to the actual Ap measurements are also discussed.

The primary data processing of the neutron monitors is a necessary procedure in order to provide the worldwide network of neutron monitors with high quality data. The procedure should be performed in a real time code which means that it should be fast and make use only of the past measurements of a neutron monitor. In general, the data correction algorithms are based on the comparison among the different channels of the detectors. Such methods, which are used currently by the Athens neutron monitor station as well as by many other stations are the Median Editor and the Super Editor. In this work, two new algorithms that are currently being developed in the Athens Station are presented. The first one is based on an Artificial Neural Network model, while the second one is based on a pure statistical model.

Using as a parameter the average difference between the heliocentric longitudes of the planets Venus, Earth and Jupiter, the strong link of 22-year and 11-year cycles of solar activity with the lowest values of the parameter have been found. The envelope curve of the minimum values of this parameter describes well both the conjunctions of the three planets, when they are almost in a straight line from the Sun, which causes the maximum of solar activity; and the conjunctions in larger longitudinal sector (25-30°), which occur much more frequently and are accompanied by different combinations of planets on the opposite sides from the Sun, that also causes the maximum of solar activity. The location of these planets on the opposite sides from the Sun in various combinations is well compatible with this parameter.

Using the PLANETOCOSMICS simulation framework we simulated solar proton transport through the Earth's atmosphere and estimated angular and energy distributions of secondaries (protons, electrons, positrons, muons, photons and neutrons) at various atmospheric levels. As the source spectrum of solar protons at the boundary of atmosphere the spectra obtained with the GLE modeling from the data of neutron monitor network in a number of events have been used. These Monte Carlo simulation results were compared with the available solar cosmic ray neutron monitor and balloon measurements. The calculated solar proton spectra are in good agreement with the balloon and neutron monitor observational data.

During a geomagnetic storm, many interesting variations in cosmic ray intensity recorded by the worldwide network of neutron monitor stations are observed. More specifically, a characteristic increase of cosmic ray intensity mainly in the middle latitude stations is observed, due to the geomagnetic cut-off rigidity changes. During the declining phase of the last solar cycle, many characteristic geomagnetic effects were observed with the most significant one on November of 2003, which is considered as the largest magnetic storm in the history of neutron monitors. In this work, the magnetic storms of 31 March 2001, 11 April 2001, 8 and 10 November 2004, 15 May 2005 and 24 August 2005 are analyzed using cosmic ray data from a number of neutron monitor stations located at different places worldwide.

The first significant Forbush decrease of solar cycle 24 was recorded in February 18, 2011 from neutron monitors around the world. This was the result of the coronal mass ejections (CMEs) that was released from the Sun on 14 and 15 February 2011, respectively, and their interplanetary counterparts (ICME) that were prevalent in the interplanetary space in this period. We report on the global characteristics of cosmic rays during the FD such as the amplitude (A0), the decrement and the three dimensional anisotropy parameters (Ax, Ay and Az), deduced from the global survey method (GSM). We also analyze the interplanetary space solar wind data and we present the structure of the ICME as it passed through the Earth resulting in a strong Forbush decrease. We compare high time resolution neutron monitor data with multipoint space-based measurements of the interplanetary space (e.g. ACE/SWEPAM and ACE/MAG).

Solar proton events during a period from 1956 to 2012 are considered. Fluences of protons of various energies in these events have been computed. On the basis of these extensive data the inhomogeneity of the distribution of their sources on the Sun along the Carrington longitude has been confirmed, which had been earlier revealed in our studies. Special attention is paid to the discovered interval of "passive longitudes", extensive over the longitude (90-170°) and the life time (the whole period of observations). The summarized proton fluence of the events, which sources belong to this interval of Carrington longitudes, is considerably lower, than the summarized proton fluences of the events in the other heliolongitude intervals. From the 60 most powerful solar proton events during the whole period of observations not more than 1 event has been originated from this interval of "passive longitudes".

Basing on the data of AVS-F apparatus from SONG-D detector onboard CORONAS-F satellite, we have studied the extreme solar event of January 20, 2005 used the 2.223 MeV, 4.44 MeV and 6.13 MeV γ-lines temporal profiles. By the statistical modeling method we calculated the temporal profile of 2.223 MeV line too. Calculations have been performed in assumption of Bessel type of accelerated particles energy spectrum, different ³He content in the region of nuclear reactions and several density models of the solar atmosphere. Comparisons of the results of modeling with observational 2.223 MeV AVS-F/SONG-D data reveal the increasing of the ratio of ³He concentration to ¹H one during the flare from 2× 10–⁵ at the rise phase of the gamma-ray flux up to 2× 10^−-4 at the decay one. During the same period the spectrum became harder and the density of solar atmosphere increased too. Averaged over full time of 2.223 MeV γ-emission concentration ratio of ³He/¹H is equal to (1.40±0.15)×10^−-4, also the density model with enlarged density up to 2×10¹⁷ cm⁻³ in the lower chromosphere and through the whole photosphere is realized. Besides, we have estimated the spectral index αT that is close to 0.1 for accelerated protons in the range of 1-100 MeV. Using the AVS-F gamma-rays spectral data in the wide range up to 140 MeV, we have obtained the spectral index of s=2.5±0.1 in the case of power law spectrum for energies more than 300 MeV.

Analysis of long-term observations of the fluxes of interplanetary protons with energies from >1 to >100 MeV measured at a distance of 1 AU from the Sun has been carried out. The results of computations of the maximal, average and minimal values of total interplanetary proton fluences accumulated over the periods from 1 month to 10 years are presented. Possibilities of application of the obtained data for the characterization and prediction of space weather and climate are discussed.

The beginning of 2012 is characterized by a burst in solar activity, which is especially obvious, in the first half of March. During these days a series of considerable solar flares was observed – among which six of great significance – together with several powerful emissions of solar substance (coronal mass ejections – CMEs) which resulted in large solar wind disturbances. As a result, several magnetic storms ranging from minor to severe were registered at the Earth. The splash in solar activity was also revealed in cosmic rays. Specifically, on January 27th and on March 7th, 13 significant proton increases (solar energetic particle – SEP) at several spacecrafts and instruments which probably were accompanied by very small ground level enhancements (GLEs) were observed. Furthermore, a series of Forbush decreases is recorded in the same time (i.e. March 2012). It is worth noting that the Forbush decrease on March, 7th became the greatest (up to now) event of its kind in the new cycle of solar activity. All of the aforementioned cosmic rays phenomena are investigated in the given work on the basis of the data from the worldwide network of neutron monitors.

The history of cosmic ray study by means of ground-based methods in the 1930s contains some gaps. The press barely covered the study of cosmic rays at the "Urusvati» Himalayan Research Institute that functioned in the Indian Himalayas in 1928-1939. Archival materials of the "Urusvati" Institute now stored at the International Centre-Museum named after N.K. Roerich (Moscow), give evidence to the active participation of the Institute staff in the study of cosmic rays. By the initiative of A.H. Compton, in 1932 several expeditions on the studies of cosmic rays were organized in different parts of the world. One of these expeditions passed through the Himalayas in the region of the South-Eastern Ladakh. The report on this highland expedition which took place at the altitude of 19,500 feet above the sea level was published by J.M. Benade in the "Urusvati Journal" (was issued during 1931-1933). Cooperation between George Roerich, the Institute Director, and Prof. J.M. Benade in expedition to Ladakh has been documented.

Theoretical considerations concerning of the charged particles acceleration in general, and in particular, the peculiarities of protons acceleration in the Neutral Layer of Cosmic Space, in the frame of Maxwell Electro-Magnetic Field Theory have been reviewed on the article. A brief historical review of events is given, indicating that protons can be speeding up to ultra-relativistic energies in the Neutral Layer of the Interplanetary Magnetic Field, which is affirmed by anomalously high number of cosmic μ-mesons, generated by protons, through the decay of π- and -mesons, have been discovered in lower layers of the Earth's Atmosphere, as well as in a great depths of underground

The largest uncertainties in a numerical simulation of cosmic ray induced atmospheric cascade are due to hadron interaction models. The influence of low energy hadron interaction models in CORSIKA code on longitudinal cascade development is important. It results longitudinal cascade development, respectively energy deposit and atmospheric ionization by secondary particles. In this work are presented simulations with CORSIKA 6.990 code using GHEISHA 2000, FLUKA 2011 and QGSJET II hadron generators. The energy deposit in the atmosphere by various nuclei, namely Helium, Oxygen and Iron is calculated. The ion pair production in the atmosphere and the impact of the different shower components, precisely the electromagnetic, muon and hadron is estimated according the used hadron generators. The yield function Y for total ionization is compared for various cases. The observed differences and applications are discussed.

We consider bursts in the neutrons registered by the Yakut spectrograph of cosmic rays and the electrostatic fluxmeter (± 50 kV/m). Bursts were observed during a significant change in the field, which changes abruptly from − 16 kV/m to 18 kV/m during negative lightning. It was found that during the positive lightning have not been observed bursts of neutrons, despite that the electric field changes abruptly from 10 kV/m up to −30 kV/m during the lightning discharge.

The study of the contribution of high energy particles of galactic and solar origin to cosmic ray induced ionization in the atmosphere of the Earth is of a big interest. The ion production rates in the atmosphere of the Earth due to a major solar energetic particle events on 28 October 2003 and 20 January 2005 produced by solar protons are obtained. The proton spectra are considered on the basis of GOES 11 satellite measurements and bibliographic data. The Forbush decrease during GLE 69 is taken into account. The cosmic ray induced atmospheric cascade simulation is carried out with CORSIKA 6.990 code using FLUKA 2011 and QGSJET II hadron interaction models. During the simulation a winter profile of the atmosphere is considered, which permits realistic description of the event. The ion production rate is compared for 40 N, 60 N and 80 N latitudes. The time evolution of obtained ion rates is presented. The 24h ionization effect is for various latitudes. It is demonstrated that the ionization effect is important on sub-polar and polar latitudes. The obtained results are discussed.

The COsmic Ray Ionization Model for Ionosphere and Atmosphere (CORIMIA) is physical space weather model with fully operational implementations. CORIMIA produce values of electron production for different altitudes (30 – 120 km), solar activities (low, moderate and high), geomagnetic and atmospheric cut offs. CORIMIA can determine the energy intervals contributions for all groups of CR nuclei. The effects of galactic cosmic rays (GCR), solar cosmic rays (SCR) and anomalous cosmic rays (ACR) in the middle atmosphere are computed. The structure of the proposed model allows its decomposition in several submodels. Each submodel is further decomposed in submodels with account to the different characteristic ionization losses energy intervals. The ionization losses function is calculated taking into account the energetic particles charge decrease interval. The energy intervals investigation takes place according to the goal of the user of the model with respect to accuracy and interval types. CORIMIA program is applicable for the ionosphere and atmosphere above 30 km. Below this altitude numerical model such as CORSIKA are applied. At present the composite CORIMIA – CORSIKA programs are used.

Since 1957 the Lebedev Physical Institute has being performed observations of ionizing radiation in the atmosphere from the ground level up to the height of 30-35 km. The time series of charged particle fluxes in the near-ground levels of the atmosphere at polar latitudes and at mid-latitude obtained in the course of the experiment are presented. The measured fluxes include cosmic ray particles and radioactivity. Over the solid ground radioactivity is observed up to the heights of ∼ 3 km. Over the sea surface radioactivity level is several times less than over the solid ground. It seems that above the ground surface up to ~1.5 km there is a contribution from the cosmic ray air-soil transition effect.